An investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data
Klaus Bernhard, Sebastián Otero, Stefan Hümmerich, Nadejda Kaltcheva, Ernst Paunzen, Terry Bohlsen
MMNRAS , 1–46 (2017) Preprint 30 May 2018 Compiled using MNRAS L A TEX style file v3.0
An investigation of the photometric variability of confirmed andcandidate Galactic Be stars using ASAS-3 data
Klaus Bernhard, , ⋆ Sebastián Otero, Stefan Hümmerich, , Nadejda Kaltcheva, Ernst Paunzen, Terry Bohlsen American Association of Variable Star Observers (AAVSO), 49 Bay State Rd, Cambridge, MA 02138, USA Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne e.V. (BAV), Munsterdamm 90, D-12169 Berlin, Germany Department of Physics and Astronomy, University of Wisconsin Oshkosh, 800 Algoma Boulevard, Oshkosh, WI 54901, USA Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlářská 2, 611 37 Brno, Czech Republic Mirranook Observatory, Boorolong Rd, Armidale, NSW, 2350, Australia
Accepted XXX. Received YYY; in original form ZZZ
ABSTRACT
We present an investigation of a large sample of confirmed ( N =233) and candidate ( N =54)Galactic classical Be stars (mean V magnitude range of 6.4 to 12.6 mag), with the mainaim of characterizing their photometric variability. Our sample stars were preselected amongearly-type variables using light curve morphology criteria. Spectroscopic information wasgleaned from the literature, and archival and newly-acquired spectra. Photometric variabilitywas analyzed using archival ASAS-3 time series data. To enable a comparison of results,we have largely adopted the methodology of Labadie-Bartz et al. (2017), who carried out asimilar investigation based on KELT data. Complex photometric variations were establishedin most stars: outbursts on different time-scales (in 73 ± ± ± ± ± Key words:
Stars: early-type – stars: emission-line, Be – stars: circumstellar matter – stars:variables: general – stars: oscillations
According to the still widely-employed definition by Jaschek et al.(1981), Be stars are non-supergiant B stars whose spectra show, orhave shown at some time, emission in one or more of the hydrogenBalmer lines. While useful for initial classification, this definitionis very broad and does not take into account the underlying mecha-nism responsible for the observed line emission, which is a generalsignature of circumstellar gas of a certain density. Thus, Balmerline emission may be observed in very different and not neces-sarily related objects like e.g. Herbig Ae/Be stars (Rivinius et al.2013). Another, regularly-observed spectroscopic characteristic of ⋆ E-mail: [email protected]
Be stars is the presence of singly-ionized metal lines, like e.g. Fe II(Hanuschik 1994; Gray & Corbally 2009).The focus of the present investigation is on the ’classical Bestars’, a term that has recently been employed to exclude otheremission-line objects like mass-transferring binary systems andHerbig Ae/Be stars (Porter & Rivinius 2003; Subramaniam et al.2012). These stars are rapidly-rotating main-sequence B objectsnotorious for forming gaseous, outwardly-diffusing Keplerian disks(Rivinius et al. 2013) that may develop and disperse on time-scales If not indicated otherwise, here and throughout the paper, the term Bestars always refers to the classical Be stars.© 2017 The Authors a r X i v : . [ a s t r o - ph . S R ] M a y Bernhard et al. of months to years. Cases are known in which a ’regular’ B star,which has never shown any signs of emission, suddenly develops adisk, as has been observed in e.g. ω Ori and δ Sco (Guinan & Hayes1984; Fabregat et al. 2000). Discovered more than 150 years ago(Secchi 1866), Be stars still present puzzles to astronomers, al-though recent decades have seen significant advances.Be stars exhibit complex variability on very different time-scales ranging from a few minutes to decades (Sterken et al. 1996;Labadie-Bartz et al. 2017, LB17 hereafter). Studying these varia-tions is important to derive information on the (interplay of) as-trophysical phenomena involved. Short-term variability in Be starshas been commonly observed in ground-based photometric stud-ies, especially among earlier spectral types (Cuypers et al. 1989;Hubert & Floquet 1998). However, only with the advent of high-precision space photometry, it has become clear that, apparently,short-term variability is ubiquitous in these stars and rich frequencyspectra have been observed in many objects (Gutiérrez-Soto et al.2007; Emilio et al. 2010; Rivinius et al. 2017).Periodic variations on intermediate time-scales (days tomonths) have also been reported in Be stars. For example,Mennickent et al. (1994) and Sterken et al. (1996) have establishedthe existence of periodic and quasi-periodic variability in several Bestars on time-scales between days and months. Non-radial pulsationcannot be reconciled with these long periods, although the beatingof closely-spaced non-radial pulsation frequencies has been postu-lated as a possible explanation (Sterken et al. 1996; LB17). Binarityand disk-related phenomena (e.g. the propagation of density wavesin the disk) can also lead to this kind of variations (Rivinius et al.2013), and outbursts may (re)occur on similar time-scales. Studieswith the BRITE satellites have drawn a more differentiated pictureand shown that several mechanisms might be at work in a singlestar (Baade et al. 2017a).Photometric variability on long time-scales (months todecades) are generally attributed to (changes in) the circumstellardisk, most notably its development and dispersion. Disks are createdthrough events referred to as outbursts, in which mass is elevatedfrom the stellar surface and the development of, and mass-transferto, the disk is initiated. Outbursts are accompanied by characteristicphotometric variations. Depending on the inclination angle of thesystem, the object may get brighter or dimmer (Haubois et al. 2012).When seen pole-on, the resulting energy distribution will be that ofthe stellar continuum plus excess from the colder (and hence red-der) disk (’Be phase’). At visual wavelengths, brightenings of up to ∼ The lower limit can be much shorter. For example, Peters (1986) reportedthe development of H α emission in the transient Be star µ Cen in only twodays. See also Baade et al. (1988).
The development of Be star disks, which have become knownas ’decretion disks’ (Pringle 1992), is rather well understood; oncematter has been ejected, it is governed by viscous processes. How-ever, the mechanism(s) behind the formation and maintaining of thecircumstellar disks in Be stars have remained elusive. Be stars arefast rotators (rotation rate of about 75 % of critical or above). How-ever, the majority of them likely does not achieve critical rotationrates (critical rotation in Be stars has been initially suggested byStruve 1931), and a mechanism besides rotation is needed to triggerthe ’Be phenomenon’. Be star disks are known to form and dissipateover relatively short time scales, which are too short to be related tostellar evolutionary effects. Whatever mechanism is operating musttherefore be capable of switching on and off (Rivinius et al. 2013).The most promising mechanism in this respect is pulsation.While pulsation was suggested as a potential trigger of mass loss inBe stars at an early stage (Baade 1988), it has remained open for along time whether the short-period variability ( P < 2.0 d) observedin Be stars is due to rotational modulation (Balona 1990) or pulsation(Baade 1987, see e.g. the discussion in Porter & Rivinius 2003).Recent evidence strongly favours the scenario that all Be stars are infact non-radially pulsating stars (Semaan et al. 2011; Rivinius et al.2013; Baade et al. 2017a).While single non-radial pulsation modes are not suited totrigger mass loss, beating effects may produce higher amplitudes(Neiner et al. 2002; Rivinius et al. 2013; Labadie-Bartz et al. 2017)and a connection between pulsational amplitude and circumstel-lar activity has been established (Carciofi et al. 2008; Neiner et al.2013). Interestingly, so-called ’difference frequencies’ ( ∆ frequen-cies) may show amplitudes in excess of the amplitude sum of theirassociated pulsational base frequencies, influencing the mass trans-fer to the circumstellar environment (Baade et al. 2016, 2017a,b).In summary, compelling evidence now exists that pulsation is at theroot of the mass ejection events observed in Be stars.Many reviews on Be stars have been published, and we do notattempt to give an exhaustive overview. For a summary of the earlierliterature, the reader is referred to Underhill & Doazan (1982), whileRivinius et al. (2013) provide an excellent survey of the currentknowledge.The present work presents an investigation of a large sampleof confirmed ( N = 233) and candidate ( N = 54) Galactic Be stars,using archival photometric and spectroscopic observations as wellas newly-acquired spectra, with the main aim of describing theirphotometric variability. Our methodological approach is outlinedin Section 2. Results are presented in Section 3 and discussed inSection 4. Our sample was initially recruited from a list of early-type variablestars compiled by one of us (S.O.), which was assembled by a sys-tematic investigation of photometric time series data from the AllSky Automated Survey (Pojmański 2002, ASAS hereafter) archive.To this end, the light curves of bright objects ( V T < ∼ . mag) withsuitable Tycho-2 colours (( B T − V T ) < ∼ . mag; Høg et al. 2000)were visually inspected using a semi-automated approach. The em-phasis was on discovering new variables; therefore, objects withwell-defined variability types contained in catalogues like the Gen-eral Catalogue of Variable Stars (GCVS; Samus et al. 2017) andthe International Variable Star Index (VSX) of the American As-sociation of Variable Star Observers (Watson 2006) were rejected. MNRAS000
The development of Be star disks, which have become knownas ’decretion disks’ (Pringle 1992), is rather well understood; oncematter has been ejected, it is governed by viscous processes. How-ever, the mechanism(s) behind the formation and maintaining of thecircumstellar disks in Be stars have remained elusive. Be stars arefast rotators (rotation rate of about 75 % of critical or above). How-ever, the majority of them likely does not achieve critical rotationrates (critical rotation in Be stars has been initially suggested byStruve 1931), and a mechanism besides rotation is needed to triggerthe ’Be phenomenon’. Be star disks are known to form and dissipateover relatively short time scales, which are too short to be related tostellar evolutionary effects. Whatever mechanism is operating musttherefore be capable of switching on and off (Rivinius et al. 2013).The most promising mechanism in this respect is pulsation.While pulsation was suggested as a potential trigger of mass loss inBe stars at an early stage (Baade 1988), it has remained open for along time whether the short-period variability ( P < 2.0 d) observedin Be stars is due to rotational modulation (Balona 1990) or pulsation(Baade 1987, see e.g. the discussion in Porter & Rivinius 2003).Recent evidence strongly favours the scenario that all Be stars are infact non-radially pulsating stars (Semaan et al. 2011; Rivinius et al.2013; Baade et al. 2017a).While single non-radial pulsation modes are not suited totrigger mass loss, beating effects may produce higher amplitudes(Neiner et al. 2002; Rivinius et al. 2013; Labadie-Bartz et al. 2017)and a connection between pulsational amplitude and circumstel-lar activity has been established (Carciofi et al. 2008; Neiner et al.2013). Interestingly, so-called ’difference frequencies’ ( ∆ frequen-cies) may show amplitudes in excess of the amplitude sum of theirassociated pulsational base frequencies, influencing the mass trans-fer to the circumstellar environment (Baade et al. 2016, 2017a,b).In summary, compelling evidence now exists that pulsation is at theroot of the mass ejection events observed in Be stars.Many reviews on Be stars have been published, and we do notattempt to give an exhaustive overview. For a summary of the earlierliterature, the reader is referred to Underhill & Doazan (1982), whileRivinius et al. (2013) provide an excellent survey of the currentknowledge.The present work presents an investigation of a large sampleof confirmed ( N = 233) and candidate ( N = 54) Galactic Be stars,using archival photometric and spectroscopic observations as wellas newly-acquired spectra, with the main aim of describing theirphotometric variability. Our methodological approach is outlinedin Section 2. Results are presented in Section 3 and discussed inSection 4. Our sample was initially recruited from a list of early-type variablestars compiled by one of us (S.O.), which was assembled by a sys-tematic investigation of photometric time series data from the AllSky Automated Survey (Pojmański 2002, ASAS hereafter) archive.To this end, the light curves of bright objects ( V T < ∼ . mag) withsuitable Tycho-2 colours (( B T − V T ) < ∼ . mag; Høg et al. 2000)were visually inspected using a semi-automated approach. The em-phasis was on discovering new variables; therefore, objects withwell-defined variability types contained in catalogues like the Gen-eral Catalogue of Variable Stars (GCVS; Samus et al. 2017) andthe International Variable Star Index (VSX) of the American As-sociation of Variable Star Observers (Watson 2006) were rejected. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Suspected or misclassified variables and variables of undeterminedor doubtful type were kept.To build up an initial sample of classical Be stars for the presentstudy, the resulting list of objects was searched for objects exhibit-ing a variability pattern in agreement with a Be star classification.To guide us in this endeavor, we have employed the variability typesdeveloped by LB17 to describe the diverse manifestations of photo-metric variability in these stars. In summary, the light curves weresearched for the presence of the following variations, which are dis-cussed in more detail in Section 3.2 (the corresponding LB17 typesare provided in parentheses):a) long-term changes in mean brightness on the order of years todecades (type LTV),b) outburst variation, i.e. a sudden change in flux that is followedby a (generally) more gradual decline to baseline brightness (typeObV),c) periodic variations on intermediate time-scales of days tomonths (type IP),d) short-period variability (defined as periodic variability with P ≤ d by LB17; type NRP).Be stars often exhibit several or all of the above-listed types ofvariation in their light curves (LB17). It is therefore reasonable toexpect complex light changes during the nearly 10 years of ASAS-3coverage. (As can be seen from the set of light curves provided inFig. B1, the results of our study have subsequently shown that this isindeed a reasonable assumption.) Similar complex light variationsare not expected in most other variable stars in the outlined spectralrange, such as β Cep stars, slowly-pulsating B (SPB) stars or α Canum Venaticorum variables, which especially holds true for thelarge-amplitude outbursts and long-term mean magnitude changesobserved in Be stars. Therefore, attention was paid in particular toitems a) and b).In this way, the light curves of all objects exhibiting a variabilityamplitude of at least 0.05 mag were subjected to a careful visualinspection, in agreement with the approach of LB17. A specificvariability type was only registered if it could be clearly identifiedin the light curve.301 objects were preselected in this way and further in-vestigated using literature information gleaned from the SIM-BAD (Wenger et al. 2000) and VizieR (Ochsenbein et al. 2000)databases. 239 stars could be confirmed as emission-line stars bytheir spectral type(s) in the literature (cf. the spectral types givenin Table A1). We note that although Be stars are non-supergiantobjects by definition, we a priori decided to only exclude stars ofluminosity type Ia. This decision has been made in order to takeinto account the great uncertainty in (luminosity) classification thatexists among a significant part of our sample stars. Indeed, as dis-cussed in Section 2.3, the variable nature of Be star spectra resultsin a great range of listed spectral types for some objects.As the focus of the present investigation is on the classical Bestars (cf. Section 1), care was taken to exclude B[e] stars and HerbigAe/Be stars. To this end, the literature was searched for classificatoryinformation, and a very few B[e] stars that had been selected for theinitial sample were thus subsequently removed. In the case of theHerbig Ae/Be stars, a two-fold approach was taken that relied onliterature information and colour-colour plots. It has been shown thatHerbig Ae/Be stars can be efficiently distinguished from classical Bestars at infrared wavelengths (Rivinius et al. 2013), as they generallyexhibit significant infrared excesses due to the presence of dust inthe circumstellar environment. The disks of classical Be stars, on the other hand, contain no dust; the observed infrared excess in theseobjects is due to free-free radiation of hydrogen.We have therefore investigated our sample stars using infraredobservations from the 2MASS (Skrutskie et al. 2006) and WISE(Wright et al. 2010) catalogues and investigated all stars with sig-nificant near-infared (( J − K ) − ( B − V ) > ∼ V − [ ] > ∼ mag) excesses. Most of these objects were found toshow peculiar light curves and have been classified at least onceas young stellar objects in the literature. Furthermore, we checkedfor the presence of diffuse nebulae by a visual inspection of thecorresponding WISE images using the ALADIN visualization tool(Bonnarel et al. 2000). The presence of diffuse nebulae was revealedin all cases. Consequently, these objects were assumed to be HerbigAe/Be stars and removed from the sample.Only two eclipsing binary systems are present in our sample,which – judging from their light curves – might be detached systemsharbouring classical Be stars. We have chosen to keep them in thesample, in accordance with the approach of LB17. We also searchedfor the possible presence of cataclysmic variables, which are easilyrevealed by their infrared colours (contribution of the donor star)and X-ray properties, but no such objects were found.In addition to the classifications in the literature, some furtherobjects could be confirmed by LAMOST spectra, our own spectraand uvby β photometry. All in all, 233 classical Be stars were selectedin this way. The high detection rate indicates that our selectioncriteria based on light curve morphology are a viable and efficientmethod of identifying classical Be stars among early-type stars inlarge photometric time-series databases. We therefore felt justifiedin including the remaining 54 stars as candidate Be stars into thefinal sample. These stars exhibit a variability pattern in agreementwith a classical Be star classification but have never been identifiedas emission-line objects in the literature. As it is not uncommonfor Be star disks to (re)appear and disperse on time-scales thatmay reach years or decades, a Be star need not necessarily showemission at all epochs. It is thus possible that Be stars have beenmissed in spectroscopic surveys if they did not show emission at thecorresponding epoch of observation.In summary, the final sample encompasses 287 stars – 233spectroscopically-confirmed Be stars and 54 Be star candidates inthe mean V magnitude range of 6.4 to 12.6 mag that were selectedby light curve morphology criteria. For convenience, all stars werenumbered in order of increasing right ascension (No. 1 – No. 287).Throughout this study, in the discussion of stars of interest, theinternal identification number is always listed in parentheses, inorder to provide an easy identification in the corresponding tables.The distribution of our sample stars in Galactic coordinates isshown in Fig. 1, together with the sample of LB17. As expected, Bestars are mostly confined to the Galactic disk. There is an obviousgap in the distribution of our sample stars (from l ≈ ◦ to l ≈ ◦ ).This is due to the fact that in the outlined RA range, the Galacticdisk reaches declinations northerly of +28 ◦ , which is outside thecoverage of our photometric data source (cf. Section 2.4). During the preparatory stages of our investigation, LB17 published athorough analysis of the photometric variability of Be stars employ-ing observations from the Kilodegree Extremely Little Telescope(KELT; Pepper et al. 2007) transit survey. To this end, well-knownBe stars from the Be Star Spectra (BeSS) database (Neiner et al.2011) were chosen and cross-matched with entries in the KELTdatabase, which resulted in a sample of 610 stars. Because of sig-
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Bernhard et al.
Figure 1.
Distribution in Galactic coordinates of our sample (black dots)and the sample of LB17 (grey dots). The obvious gap in the distribution ofour sample stars in the right-ascension (RA) interval from l ≈ ◦ to l ≈ ◦ is due to the coverage of our photometric data source (cf. Section 2.4). Bothsamples complement each other well; together, they cover approximately thewhole Galactic disk. nificant saturation effects in the light curves, 510 objects were finallyincluded into the analysis. These objects are situated in the mean V magnitude range of 6.0 to 12.8 mag. KELT data boast coverage upto ∼
10 yr (although only 217 objects of the LB17 study exhibit atime baseline exceeding four years; cf. also Section 4) and have atypical sampling cadence of 30 min. The typical photometric errorfor the KELT data is 7 mmag (LB17).LB17 investigated the presence and occurrence rate of out-bursts, long-term variability related to the circumstellar disk andnon-radial pulsations. Their work therefore shares the same aimas our study, viz. the investigation of the photometric variabilityof classical Be stars. In order to enable a comparison of results,we have chosen to adopt the aforementioned authors’ methodologywherever appropriate. Thus, in the following chapters dealing withthe photometric analysis, relevant results from LB17 are mentioned,employed for comparison and included into our analysis. This ap-proach was chosen because we think that the resulting enlarged andhomogeneous sample of Be stars with known properties will fa-cilitate further research on these objects and thereby serve the Bestar community best. We stress, however, that the validity of thiscomparison is severely compromised by the different data sourcesemployed and the different ways the samples were compiled.
When investigating Be stars, it is useful to subdivide thesample into early-type, mid-type and late-type Be stars (e.g.Gutiérrez-Soto et al. 2007). We have divided our sample accord-ing to the scheme employed by LB17 and consider Be stars withspectral types earlier than B4 as early-type Be stars , objects withspectral types of B4, B5 and B6 as mid-type Be stars , and stars withspectral type of B7 and later as late-type Be stars . Objects withouta specific spectral type in the literature are listed as unclassified Bestars .The spectroscopic classification of our target stars was gleanedfrom various literature sources, which are listed in the presentationof results in Table 2. Spectra from the BeSS database were also se-cured and primarily used to check the literature types and to searchfor the presence of emission lines. For some of our stars, spectrafrom the LAMOST DR2 archive (Cui et al. 2012; Luo et al. 2016)are available, which were also taken into consideration (Figure C1).Additional spectra of several of our target stars (unclassified or ambiguously classified objects with few or no spectroscopic ob-servations in the BeSS database or the literature) were obtainedat Mirranook Observatory using a LISA spectrograph on a C11279/2800 mm Schmidt-Cassegrain telescope. The LISA is a com-mercially available classic spectrograph optimised for 400-700 µ mand was used with a 23 µ m slit. The employed camera is an Atik314+ cooled CCD camera with 6.45 µ m pixels giving well sam-pled images with a 23 µ m slit. The spectra taken had a S/N ≈ ≈ ASAS is a photometric survey which aims at the detection and in-vestigation of all kinds of photometric variability. ASAS constantlymonitored the entire southern sky and part of the northern sky up toa declination of about δ < +28 ◦ . Most data were acquired during thethird phase of the project, ASAS-3, which lasted from 2000 until2009 (Pojmański 2002). The ASAS instruments were situated atthe 10-inch astrograph dome of the Las Campanas Observatory inChile and consisted of two wide-field telescopes equipped with f/2.8200 mm Minolta lenses and 2048 x 2048 AP 10 Apogee detectors.A sky coverage of 8 . ◦ . ◦ . ′′ ′′ for bright stars and up to 15.5 ′′ for fainter objects. Therefore,blending issues arise and photometry is rather uncertain in crowdedfields such as star clusters.ASAS monitored about 10 sources in the magnitude rangebetween the saturation limit V = 7 (up to V ≈ V =14. During To our knowledge, the literature does not provide any information onwhether detector saturation or A/D saturation is involved. Consulting themanual of the employed CCD cameras, we strongly suggest that the formerholds true. MNRAS000
When investigating Be stars, it is useful to subdivide thesample into early-type, mid-type and late-type Be stars (e.g.Gutiérrez-Soto et al. 2007). We have divided our sample accord-ing to the scheme employed by LB17 and consider Be stars withspectral types earlier than B4 as early-type Be stars , objects withspectral types of B4, B5 and B6 as mid-type Be stars , and stars withspectral type of B7 and later as late-type Be stars . Objects withouta specific spectral type in the literature are listed as unclassified Bestars .The spectroscopic classification of our target stars was gleanedfrom various literature sources, which are listed in the presentationof results in Table 2. Spectra from the BeSS database were also se-cured and primarily used to check the literature types and to searchfor the presence of emission lines. For some of our stars, spectrafrom the LAMOST DR2 archive (Cui et al. 2012; Luo et al. 2016)are available, which were also taken into consideration (Figure C1).Additional spectra of several of our target stars (unclassified or ambiguously classified objects with few or no spectroscopic ob-servations in the BeSS database or the literature) were obtainedat Mirranook Observatory using a LISA spectrograph on a C11279/2800 mm Schmidt-Cassegrain telescope. The LISA is a com-mercially available classic spectrograph optimised for 400-700 µ mand was used with a 23 µ m slit. The employed camera is an Atik314+ cooled CCD camera with 6.45 µ m pixels giving well sam-pled images with a 23 µ m slit. The spectra taken had a S/N ≈ ≈ ASAS is a photometric survey which aims at the detection and in-vestigation of all kinds of photometric variability. ASAS constantlymonitored the entire southern sky and part of the northern sky up toa declination of about δ < +28 ◦ . Most data were acquired during thethird phase of the project, ASAS-3, which lasted from 2000 until2009 (Pojmański 2002). The ASAS instruments were situated atthe 10-inch astrograph dome of the Las Campanas Observatory inChile and consisted of two wide-field telescopes equipped with f/2.8200 mm Minolta lenses and 2048 x 2048 AP 10 Apogee detectors.A sky coverage of 8 . ◦ . ◦ . ′′ ′′ for bright stars and up to 15.5 ′′ for fainter objects. Therefore,blending issues arise and photometry is rather uncertain in crowdedfields such as star clusters.ASAS monitored about 10 sources in the magnitude rangebetween the saturation limit V = 7 (up to V ≈ V =14. During To our knowledge, the literature does not provide any information onwhether detector saturation or A/D saturation is involved. Consulting themanual of the employed CCD cameras, we strongly suggest that the formerholds true. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data the third project phase, observations were acquired in the Johnson V passband. The typical scatter of an observation in the magnituderange 8 < ∼ V < ∼
10 is about 0.01 mag (e.g. Pigulski 2014). Becauseof the long time baseline of the project, the detection of periodicsignals with very small amplitudes is possible. Periodic signals withamplitudes as low as ∼ − typically amounts to 3-5 mmag(cf. in particular their Fig. 16).ASAS maintained a rather strict observing cadence, which re-sults in strong daily aliasing. A field was typically observed one tothree times per day (Pigulski 2014), although for several stars, ob-servations up to five times per day are available. Therefore, care hasto be taken in the interpretation of the resulting Fourier amplitudespectra. Pigulski & Pojmański (2008) used ASAS-3 data to investi-gate a sample of β Cep stars and identified periodic variability downto periods of the order of ∼ Data of our target stars were downloaded from the ASAS-3 web-site. Data points with a quality flag of ’D’ (=’worst data, probablyuseless’) were removed and all light curves were inspected visually.Obvious outliers and data points associated to exceedingly large er-ror bars were deleted. As the removal of only a few datapoints mayhave a significant impact on the frequency analysis, care was takenin this process.While the majority part of ASAS-3 datasets is homogeneousand of good quality, several issues exist that may render ASAS-3datasets unreliable (cf. the discussion in David et al. 2014). Sig-nificant additional scatter might be present due to flux contribu-tion from one or more near-by objects (’blending’). Furthermore, adataset may contain exposures suffering from saturation effects, andscatter may be introduced by a star’s position close to the edge ofthe CCD. Unfortunately, concerning the latter issue, no informationis provided in ASAS data, so its impact cannot be estimated. SomeASAS datasets are affected by instrumental long-term trends of lowamplitude, which might introduce spurious signals and mimic thelong-term variations seen in Be stars. These, however, are generallyof very low amplitude, unlike the long-term variability observed inmost of our sample stars.For objects brighter than V = 8.5 mag, all datasets were checkedfor saturation effects. These can be rather straightforwardly iden-tified and distinguished from intrinsic variability by a consistencycheck of the magnitudes in the five different extraction aperturesindicated by the ASAS system. Saturation is known to result insignificantly (and randomly) discrepant values between the aper-tures (David et al. 2014). Saturation was assumed to occur if themagnitude difference between the smallest aperture (2 px; ASAS-denomination ’MAG_0’) and the largest aperture (6 px; ASAS-denomination ’MAG_4’) amounted to at least 0.05 mag. This limitis an experiential value based on our own experience in dealing withthe ASAS-3 data. In consequence, datasets exhibiting a discrepancywell beyond 0.01 mag that is suspected of being attributable to sat-uration were rejected. Blending issues have been the most frequent problem we en-countered while working with the data of our programme stars.As this is not relevant to the goals of our investigation, we havenot corrected the ASAS-3 light curves presented in Fig. B1 forthe influence of close neighbouring stars. However, in order toget a clearer idea of the real amplitude of the photometric vari-ations and to provide a correct V magnitude range for catalogingpurposes, we include a corrected V range in Table 2. Dependingon the brightness of the objects, light contamination from starsas far away as 30 ′′ to 45 ′′ may affect the results. The light con-tribution of all close neighbouring stars that could be identifiedwas removed by subtracting the intensities derived from V mag-nitudes of catalogues with superior resolution. The respective V magnitudes were taken from the General Catalogue of Photomet-ric Data (GCPD; Mermilliod et al. 1997), the AAVSO PhotometricAll-Sky Survey (APASS; Henden & Munari 2014) or the Yale/SanJuan Southern Proper Motion (SPM 4.0; Girard et al. 2011) cata-logues when available. When no entry in those catalogues existed,the corresponding magnitudes were transformed from the Carls-berg Meridian Catalog 15 (CMC15; cf. Dymock & Miles 2009) orUCAC3 catalogues (UCAC3; Zacharias et al. 2010; Pavlov 2009)using 2MASS colours.The ASAS-3 magnitudes were also corrected for known zero-point offsets affecting some fields, especially in the Southern hemi-sphere. In order to do that, the closest GCPD constant field starwith a published V magnitude was selected and its magnitude com-pared with the ASAS-3 value. The differences we found range from0.00 mag in Northern fields up to 0.05 mag in far Southern fields.Column six in Table 2 lists the magnitude ranges we obtained afterapplying these corrections.Column seven indicates the total V range of the star as gleanedfrom its recorded photometric history according to data fromsources such as ASAS-3, GCPD, Hipparcos (van Leeuwen et al.1997), APASS and SPM 4.0. HIPPARCOS data have been trans-formed to Johnson V using the table in Bessell (2000). SPM 4.0magnitudes have been used only when the catalogue flags state thatthe magnitudes are derived from CCD V photometry. Comparisonsbetween APASS and GCPD data indicate that APASS is well-tiedto the standard system. We note that the ranges derived in thisway should be treated with some caution. However, the magnitudesfrom the employed sources have shown consistency with the ASAS-3 light curves spanning several years. We therefore have no reasonto suspect erroneous data in the few cases where the derived totalranges state brighter or fainter magnitudes than has actually beenobserved in ASAS-3.The search for periodic signals was done using the softwarepackage PERIOD04, which has been based on a discrete Fouriertransform algorithm and allows least-squares fitting of multiple fre-quencies to the data (Lenz & Breger 2005). In order to look forperiodic signals, the whole datasets were searched in the frequencyrealm of 0-50 d − and consecutively prewhitened with the most sig-nificant frequency, until no significant frequencies remained. In caseperiodic signals were identified, the data were folded with the result-ing frequencies and visually inspected. Only frequencies producingconvincing phase plots were kept. Aperiodic signals like long-termvariations and outbursts were identified by visual inspection. MNRAS , 1–46 (2017)
Bernhard et al.
Table 1.
Statistical information on the composition of the final sample. Weconsider Be stars with spectral types earlier than B4 as early-type Be stars ,objects with spectral types of B4, B5 and B6 as mid-type Be stars , and starswith spectral type of B7 and later as late-type Be stars .Type number (candidates thereof)early-type Be stars 101 (14)mid-type Be stars 50 (12)late-type Be stars 49 (14)unclassified Be stars 87 (14)total number 287 (54)
Table 1 gives statistical information on the composition of the finalsample. As described in Section 2.3, the division into early-type,mid-type and late-type Be stars has been based on available spectraltypes. Objects without a specific spectral type in the literature arelisted as unclassified Be stars.Table 2 presents essential data for our sample stars. We havechosen to employ GSC1.2 numbers as primary identifiers through-out the paper because they are available for all stars in our sample.Where available, more commonly used identifiers, such as HD num-bers, are given in column three of Table 2. The light curves of allobjects are presented in the Appendix (Figure B1).We have also investigated the possibilities of colour excessand intrinsic colour determination with our sample stars. As this isnot the main aim of the present work, these results have not beenemployed for the discussion of our results (cf. Section 4) and arepresented in the Appendix (Section D).
Be stars are known to exhibit long-term changes in mean brightnesson the order of years to decades. This kind of variability is linkedwith the presence or absence of the circumstellar disk, respectivelyits formation and dissipation. Emission from the disk is correlatedwith the brightness of the star. Photometric long-term variationsmay also originate in cyclic changes of the relative intensity of theviolet (V) and red (R) peaks of the Balmer emission lines (termedV/R variations), accompanied by radial velocity changes of theemissions wings and the absorption core (Harmanec 1983). Thepresence of relatively long-lived one-armed density wave patterns inthe disk may lead to cycle lengths, and hence photometric variability,on a time-scale of typically years (Okazaki 1991; Rivinius et al.2013).Exemplary light curves illustrating long-term variability areshown in Fig. 2. In most cases, the base-line of the ASAS-3 survey( ∼
10 yr) is insufficient to make a statement about the presenceof periodicity in these variations. They appear mostly aperiodic,although wave-like oscillations are present in some objects, cf. e.g.GSC 06275-00943 ( ± Figure 2.
Exemplary ASAS-3 light curves of several Be stars of the presentsample, illustrating long-term variations. The ’increased scatter’ in the lightcurve of GSC 08877-00138 ( ∼ HJD2452800, is due to short-term variations with P = 1.10487(9) d. and outbursts of very long duration (cf. Section 3.2.2) is somewhatarbitrary and, because of the limited time base of the ASAS-3 data,not always possible. LB17 have defined an outburst as a feature in the light curve delin-eated by a sharp departure from baseline brightness (either positiveor negative) followed by a (generally) gradual return towards thebaseline (cf. also Sigut & Patel 2013). While not always true, thisis a reasonable working hypothesis, as has been shown e.g. byLabadie-Bartz et al. (2018), and will be enlarged on below in thissection.Following the approach of LB17, we have searched for thepresence of outbursts in the light curves of all programme stars byvisual inspection and noted their frequency of occurrence. Severalcircumstances, however, have complicated the counting process. Be
MNRAS000
MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Table 2.
Essential data for our sample stars, sorted by increasing right ascension. The columns denote: (1) Internal identification number. Stars were numberedin order of increasing right ascension. (2) Identification from the Guide Star Catalog (GSC), version 1.2. (3) Identification from the Henry Draper (HD)catalogue or other conventional identifier. (4) Right ascension (J2000; Høg et al. 2000). (5) Declination (J2000; Høg et al. 2000). (6) V magnitude range,as derived from ASAS-3 data. Ranges that have been corrected for light contamination from close neighbouring stars (cf. Section 2.5) are marked by anasterisk. (7) V magnitude range, as gleaned from a star’s recorded photometric history (cf. Section 2.5). (8) Spectral type from the literature. (9) Subtype(E=early; M=mid; L=late; U=unclassified). (10) Emission flag (emission confirmed: l=in literature/BeSS spectra; s=in own spectra; la=in LAMOST spectra;u=from uvby β photometry). (11) variability type, following LB17: ObV=outbursts present; SRO=semi-regular outbursts; LTV=long-term variability present;NRP=non-radial pulsator candidate (periodic variability with P ≤ d); IP=intermediate periodicity (periodic variability with < P ≤ d); EB=eclipsingbinary. (12) variability type, following the GCVS and VSX classifications. (13) variability period(s), as derived from analysis of ASAS-3 data. Only part of thetable is printed here for guidance regarding its form and content. The complete table is given in the appendix (Table A1). (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)No. IDGSC IDalt α (J2000) δ (J2000) Range( V ) Range( V ) Spec.type subtype emission Var.type Var.type Period(s)[mag] lit.[mag] lit. [E/M/L/U] flag [LB17] [GCVS/VSX] [d]1 GSC06464-00405 HD29557,NSV16132 043816.174 -243930.77 8.48-8.63 8.45-8.64 B5Ib/IIp:shell?(Houk&Smith-Moore1988b),B3Ve(Levenhagen&Leister2006) M l ObV GCAS2 GSC01845-02192 HD32318,NSV16230 050317.288 +234917.46 8.39-8.63 8.38-8.63 B3IV(Straižysetal.2003),A2e(McCarthy&Treanor1965) U l ObV GCAS3 GSC08877-00138 HD33599,NSV16255 050712.946 -614818.31 8.79-9.20 8.79-9.20 B2Vep(Levenhagen&Leister2006),B5pshell(Houk&Cowley1975) M l,u ObV,NRP GCAS+LERI 1.10487(9)4 GSC04755-00818 HD293881,ASASJ051449-0310.0 051449.040 -030959.06 11.30-11.58* 11.30-11.58 B9(Cannon&Mayall1949),em(Wiramihardjaetal.1991) L l LTV GCAS5 GSC09162-00751 HD269649,ASASJ053022-6919.7 053022.553 -691938.95 10.41-10.81* 10.41-10.81 em(Howarth2012),B2.5:(Rousseauetal.1978) E l SRO GCAS6 GSC00115-01423 HD37330,NSV2478 053753.455 +005806.98 7.30-7.47 7.30-7.49 B6Vne(Warren&Hesser1978) M l,u LTV,NRP GCAS+LERI 0.77143(5)7 GSC01310-01587 HD37901,ASASJ054240+2134.7 054239.812 +213443.29 8.95-9.08 8.95-9.08 A0II/III(Hardorpetal.1965) L LTV GCAS8 GSC01311-01238 HD38191,ASASJ054456+2127.6 054456.235 +212738.48 8.42-8.74 8.42-8.74 B1:V:ne:(Morganetal.1955) E l ObV,LTV GCAS9 GSC06491-00717 HD40193,SAO171041 055622.484 -223900.05 9.15-9.30* 9.14-9.30 B8Vne:(Houk&Smith-Moore1988b),Be(Bidelman&MacConnell1973) L l ObV GCAS10 GSC01868-01264 BD+251081,ASASJ060149+2537.9 060149.500 +253752.73 10.34-10.44 10.23-10.44 OB-(McCuskey1967) U LTV GCAS star outbursts exhibit a bewildering diversity in duration, evolutionand amplitude and it is sometimes hard to differentiate whether afeature is an outburst or some other form of variability. In addition,the superposition of several types of variability and continuouslychanging baseline flux have rendered the identification difficult. Ifan outburst has not ended before another one begins (i.e. the star re-brightens before attaining baseline brightness), both outbursts weretaken into account (LB17). Generally, only stars showing unam-biguous outbursts according to the definition given above have beenconsidered. In agreement with LB17, we note that the outburstrates determined in this way are rather approximate and should beconsidered a lower limit, as outbursts with amplitudes below thedetection threshold of the ASAS-3 data will likely be present. Theoccurrence of outbursts with amplitudes on the order of ∼
10 mmaghas been established using ultra-precise space-based photometry(Balona et al. 2015). Furthermore, at an inclination angle of ∼ ◦ ,a balance between excess emission and absorption by the disk hasbeen predicted by the calculations of Haubois et al. (2012) and nonet change in optical flux is expected, although the cancellationneed not necessarily be perfect. Still, it is easily conceivable thatoutbursts will have been missed in such constellations.In this manner, outbursts were identified in 208 stars (73 ± N ob = 2.3 ± . yr − ), 33 (66 %) of mid-type Be stars (mean outburst rate of N ob = 0.7 ± . yr − ), 28 (57 %)of late-type Be stars (mean outburst rate of N ob = 0.2 ± . yr − ),and 69 (79 %) of unclassified Be stars (mean outburst rate of N ob = 1.3 ± . yr − ). A surprisingly large number of these stars(24 ± Figure 3.
Exemplary ASAS-3 light curves of several Be stars of the presentsample, illustrating outbursts of very long duration.MNRAS , 1–46 (2017)
Bernhard et al.
Figure 4.
Exemplary ASAS-3 light curves of several Be stars of the presentsample, illustrating repetitive outbursts. Note that GSC 08135-03248 ( P = 1.28212(1) d. are seen roughly pole-on and the formation of the disk results in areduced flux output of the system at visual wavelengths: instead of abrightening event, a drop in brightness is observed (cf. also Section1). Fig. 6 illustrates some characteristic examples of shell star lightcurves. Note the unusual light curve of GSC 06853-02519 ( V ).We have measured peak-to-peak amplitudes for all objects ex-hibiting outburst events and calculated corresponding mean values(Fig. 7). Although the errors are considerable, our results indicatethat the mean amplitude of outbursts decreases from early-typethrough late-type Be stars.As a next step of analysis, the time spent in outburst amongthe stars of the different sub-types was measured. The results arepresented in Fig. 8. There is an apparent tendency for earlier stars tospent more time in outburst which decreases towards later spectraltypes. However, the uncertainties are large, and the trend is notstatistically significant.Using KELT data, Labadie-Bartz et al. (2018) have correlated Figure 5.
Exemplary ASAS-3 light curves of several Be stars of the presentsample, illustrating outbursts of short duration. rising and falling times for 70 outbursts observed in 24 stars (18early-, 4 mid-, and 2 late-type Be stars). They find that the vastmajority of outburst events are indeed characterized by falling timesexceeding the rising times, with a median rising time of 8.3 d anda median falling time of 16.0 d. Interestingly, for late-type Be stars,their results indicate that the ratio of falling time to rising time issignificantly higher than for early- and mid-type objects (slope ofthe lines of best fit to the early-type, mid-type, and late-type starsare 1.97, 1.88, and 6.54, respectively). The authors conclude thattheir results suggest that, relative to the rising time, the inner diskdissipates quickly in hotter stars, and more slowly in cooler objects.They do, however, caution that their results suffer from a smallsample size and significant scatter.In order to investigate this matter with a larger sample size,we have measured rising and falling times for well-covered andwell-defined outbursts in our sample stars. In order to renderthe results comparable, we followed the methodology outlined byLabadie-Bartz et al. (2018), who measured the duration of the risingand subsequent falling phases by a close visual inspection of the light
MNRAS000
MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure 6.
Exemplary ASAS-3 light curves of several shell stars of thepresent sample, illustrating the ’negative’ outbursts typically observed inthese objects.
Figure 7.
Mean peak-to-peak amplitudes of objects exhibiting outburstsamong the different sub-types of Be stars, as derived from ASAS-3 data.
Figure 8.
Time spent in outburst among stars of the different sub-types. curve. In this way, rising and falling times were correlated for 233outbursts observed in 100 stars (41 early-, 14 mid-, 9 late-type, and36 unclassified Be stars). In accordance with Labadie-Bartz et al.(2018), we confirm that nearly all outburst events are characterizedby falling times that exceed the rising times. We find a median risingtime of 28.5 d and a median falling time of 51.0 d, and slopes of2.48, 3.35, and 2.72 for early-type, mid-type, and late-type stars,respectively.Interestingly, and in contrast to the results ofLabadie-Bartz et al. (2018), we find that a single non-linearfunction adequately describes the ratio of falling time to risingtime across all spectral subtypes, with the ratio being largerfor short events (Fig. 9). No differences were found betweenearly-, mid- and late-type stars, which suggests that the resultsof Labadie-Bartz et al. (2018) are influenced by their smallsample size, as indeed cautioned by the authors. We note that inoutburst events with short rising times up to about 65 days, thecorresponding falling times seem to be only weakly related withthe rising times.Generally, the onset of an outburst is more sharply definedthan its end; therefore, rise times are easier to determine than fallingtimes. In consequence, the errors in the estimations of the fallingtimes will be larger and may, in unfavourable cases, reach ∼
10 %.However, the employed logarithmic representation in Fig. 9 is veryrobust against measurement uncertainties, and the derived relationstill holds if we assume unrealistically high measurement errors onthe order of ∼
30 %. We are therefore confident that the observeddeviation from linearity is not caused by increased relative uncer-tainties towards longer outburst events.
Periodic variations on intermediate time-scales (days to months)are also frequently seen in Be stars. Diverse mechanisms havebeen deemed responsible for these variations, the most promis-ing and widely-accepted theories being binarity-induced variabilityand disk-related phenomena (cf. Section 1). In particular, it has beenshown that the decretion disk interacts both radiatively and gravita-tionally with the companion star (Panoglou et al. 2016, 2017).In agreement with LB17, we define variability on intermediatetime-scales (denoted as ’IP’ in Table 2) as periodic variability with < P ≤ d (cf. in particular their Table 3). Outbursts which,of course, may also (re)occur on similar time-scales, are mostlysemi-regular and have therefore been excluded from the ’IP’ class.We have identified only four stars (1 ± MNRAS , 1–46 (2017) Bernhard et al.
Figure 9.
The duration of the rising and falling times for 233 outburstsobserved in 100 stars (41 early-, 14 mid-, 9 late-type, and 36 unclassified Bestars, as indicated in the legend). The dotted line indicates a polynomial fitof the second order, which adequately describes the ratio of falling time torising time across all spectral subtypes. type of variations in 39 % of their sample stars. However, as the am-plitudes of IP variations are generally of very low amplitude (mostly ∼
10 mmag according to the examples illustrated in LB17), this re-sult is not surprising. KELT observations are of higher accuracy(typical photometric error of about 7 mmag for a single measure-ment, as opposed to about 10 mmag for ASAS-3 data; cf. Section2.4) and boast superior temporal resolution (typical sampling ca-dence of 30 min, as opposed to mostly one to three measurementsper day for ASAS-3 data).While under favourable circumstances, periodic signals withamplitudes as low as 3 mmag are detectable in ASAS-3 data (cf.Section 2.4), the complex and often irregular variability displayedby most of our sample stars is of considerably higher amplitude,which renders the detection of the low-amplitude IP variations verydifficult - in particular in the low-cadence ASAS-3 data, which arenot favourable for identifying signals at the shorter end of the IPperiods. Consequently, the peak-to-peak amplitudes of the IP vari-ations identified in this study are on the order of 20 mmag, while IPvariations with a peak-to-peak amplitude as low as 3.2 mmag havebeen identified in KELT data (LB17). In summary, we put the ob-served discrepancy in numbers down to the different characteristicsof the employed data sources.
As has been pointed out in the introduction, there is growing ev-idence that all Be stars are in fact non-radial pulsators. Some aresuspected of showing transient modes lasting for days to months,which often precede outburst events (Gutiérrez-Soto et al. 2007;Huat et al. 2009). In agreement with LB17, short period variabilityis here defined as periodic variability with P < 2 d (denoted as ’NRP’in Table 2). Evidence for the ubiquitous presence of short-periodpulsations comes mostly from ultra-precise space photometry. Pul-sations with amplitude less than 1 mmag are commonly observed,which will be missed in ground-based surveys like ASAS or KELT.In low-inclination Be stars, the variability is often dominatedby variations in the disk, which may occult the stellar variability(Baade et al. 2016) and render the detection of low-amplitude vari-ations impossible. The short period variations are also often super-imposed by complex variations with much larger amplitude, whichrenders the detection of the periodic signals difficult. Furthermore, Figure 10.
ASAS-3 light curves of two Be stars of the present sample thatexhibit variations on intermediate time-scales. The light curves of GSC08582-02609 ( P = 25.80(4) d and P = 16.77(1) d. Unless indicated otherwise,here and throughout the paper, phase plots have been based on the wholeavailable range of ASAS-3 data. the strict observing cadence of the ASAS survey (typically one tothree, and in favourable cases up to five, observations per day; cf.Pigulski 2014) is not favourable to resolving these high-frequencysignals. This may explain why we could establish short period vari-ability in only 6 ± Two eclipsing binary systems are present in our sample. GSC 08135-03248 (
MNRAS000
MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure 11.
Exemplary ASAS-3 light curves of two Be stars of the presentsample, illustrating variations on short time-scales. The light curves of GSC09196-00424 ( P = 1.14514(10) d and P = 0.483815(7) d. In order to bring outthe short-term variations more clearly, the phase plots have been based ononly part of the ASAS-3 data, as indicated below the abscissae. an orbital period of 0.84223(3) d (half the given value). However,we are confident of our period solution, as the corresponding phaseplots indicates the presence of minima of different depth.Both objects show light curve morphology in agreement witha Be star classification and, judging from their eclipse profiles andperiods, might be detached systems harbouring classical Be stars.In accordance with the approach of LB17, we have therefore chosento keep them in the sample. While we have no evidence for the pres-ence of emission features in GSC 08135-03248, uvby β photometryindicates that GSC 08975-00799 ( LB17 have correlated the observed frequency of outbursts withspectral sub-type. In agreement with the literature (Rivinius et al.2013), they have found that early-type Be stars are generally moreactive than mid-type and late-type objects. However, recent resultsbased on space photometry (Baade et al. 2016) suggest that (partof) this phenomenon may be rather due to differences in amplitudethan outburst activity. Shokry et al. (2018) confirm that late-type Bestars are generally less variable than their early-type counterparts.
Figure 12.
ASAS-3 light curve of the eclipsing binary GSC 08135-03248( P = 1.28212(1) d), respectively. Outbursts have been clipped in the lowerpanel. Figure 13.
ASAS-3 light curve of the eclipsing binary GSC 08975-00799( P = 1.68445(5) d), respectively. In order to bring out the eclipses moreclearly, the phase plot has been based on only part of the ASAS-3 data, asindicated below the abscissa.MNRAS , 1–46 (2017) Bernhard et al.
Figure 14.
Outbursts per year observed among the different sub-types of Bestars. Dark and light bars indicate, respectively, the results of this investiga-tion and LB17. The columns denoted as ’X’ give the number of stars thatdo not show definite outburst signatures in the covered time span. Note thebroken ordinates in the upper and middle panels, and the high fraction ofstars with outbursts among the unclassified Be stars, which is due to a biasin the preselection process of Be star candidates via light curve morphologycriteria (cf. Section 2.1).
However, their results indicate that the Be/B star fraction may notstrongly depend on spectral subtype and that late-type Be stars mightbe more common than is generally agreed upon.A breakdown of the number of outbursts per year observedamong the different sub-types of Be stars is provided in Fig. 14.Outburst rates have been determined as number of outbursts permonitoring interval and subsequently normalized to frequency peryear. Also included is information on the number of stars that donot exhibit outbursts in the covered time. It is obvious that a signifi-cant amount of early-type stars shows numerous outbursts per year,while mid-type and late-type objects are obviously less active inthat respect. We thus confirm the general trend that, in the accuracylimit of the employed data, early-type Be stars show more frequentoutbursts (mean outburst rate of N ob = 2.3 ± . yr − ) than mid-( N ob = 0.7 ± . yr − ) and late-type objects ( N ob = 0.2 ± . yr − ).From this figure, it is apparent that the fraction of stars withoutbursts is highest in the unclassified Be stars. This is due toa bias in the preselection process of Be star candidates via lightcurve morphology criteria (cf. Section 2.1), which favours objectsexhibiting clear Be star variability signatures, and the most dominant Figure 15.
Percentage of stars exhibiting outbursts, as derived in the presentstudy and LB17. The black bars denote the percentage of stars showingoutbursts in this study, while the grey bars indicate the percentage of starswith ≥ − in this study. The open bars represent the percent-age of stars with outbursts in LB17. Please note that for the results fromLB17, no uncertainties are available. Results are indicated for the analysisof (from left to right) early-type Be stars, mid-type Be stars, late-type Bestars, unclassified Be stars and the total sample of stars. and readily recognizable feature in this respect is the presence ofoutbursts in the light curve.However, in terms of numbers, our results differ significantlyfrom those of LB17, in particular in regard to the outburst rates ofmid-type and late-type Be stars. The discrepany in numbers is mostpronounced for objects with rare outbursts (<1 outburst yr − ; Fig.14). For example, among mid-type and late-type Be stars, LB17have identified only five such objects (cf. their Figure 1), which isin contrast to the 54 objects identified in the present study.The considerable uncertainties inherent to the counting process(cf. Section 3.2.2) might go some way in explaining the observeddiscrepancies. However, the most important aspect is surely the dif-ference in time baseline between the employed data sources. Whileboth ASAS and KELT boast coverage up to ∼
10 yr, the numberof stars actually attaining maximum temporal coverage is vastlydissimilar. LB17 find that only 217 (out of the 510 investigated)objects ( ∼
43 %) have KELT data with a time baseline exceedingfour years. In contrast, data with a time baseline of 10 yr and near-continuous sampling exist for practically all of our sample stars.Longer datasets are much more suited to the identification of Bestars with rare outbursts. In fact, most of our sample stars exhibit<1 outburst yr − (Fig. 14), with many objects showing only a singleoutburst during the ∼
10 yr of ASAS-3 coverage. These stars mayeasily have been missed in surveys with shorter time baseline. Theimpact of the time baseline on the detection of outbursts is alsoillustrated by a comparison of the vastly discrepant number of starswithout any outbursts signatures in both studies (Fig. 14).In summary, with our work, which is based on a data sourceboasting a near-continuous (albeit sparsely-sampled) coverage of ∼
10 yr for almost all sample stars, we are able to close the apparentvoid of ’rare outbursters’ proposed by LB17 and show that Be starswith infrequent outbursts are not rare.An overview over the percentage of stars that show outburstsamong the different sub-types of Be stars is provided in Fig. 15.Also illustrated are the results of LB17 (open bars), who find thatoutbursts have a higher occurrence rate in early-type stars thanin mid- and late-type objects. However, no statistically significanttrend is seen in the results for the ASAS sample (dark bars). Whilewe do find a decreasing incidence of stars showing outbursts from
MNRAS000
MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data early-type to late-type objects, the uncertainties are large, and thedistribution is essentially flat. Outbursts, therefore, are a commoncharacteristic of Be stars of all subtypes.As the longer time baseline of ASAS renders these datamore suitable to identifying objects with rare outbursts, we haverecalculated our results taking into account only objects with ≥ − (grey bars), as these frequent outbursters wouldhave been detected more easily in the shorter time-baseline KELTdata. Interestingly, the resulting distribution indeed agrees with theresults of LB17, and the difference in percentage between outburst-ing early-type and later-type Be stars is statistically significant. Ittherefore seems likely that the results of LB17 have been influencedby their data source’s bias against objects with rare outbursts.24 ± P ∼ P ∼ ± V -band have been predicted (Haubois et al. 2012). While thesepredictions seem to be accurate for the brightening events, there areseveral shell stars in our sample that exhibit drops in brightness sig-nificantly exceeding the predicted limit, most notably GSC 04826-01079 ( ∼ With our study, we significantly enlarge the sample of GalacticBe stars with a detailed description of their photometric variabilityproperties, building on the work of LB17. Wherever appropriate, wehave employed the methodological approach of the aforementionedinvestigators in order to render the results comparable. Togetherwith the results of LB17, our sample will greatly facilitate futureresearch on these objects. The main findings of the present studyare summarized in the following: • Complex photometric variations were established in most ofour sample stars: outbursts on different time-scales (in 73 ± ± ± ± • A surprisingly large number (24 ± • GSC 08135-03248 ( • Using a data source that boasts a near-continuous coverage of ∼
10 yr for almost all sample stars, we are able to close the apparentvoid of ’rare outbursters’ proposed by LB17 and show that Be starswith infrequent outbursts are not rare. • We confirm the general trend that, in the accuracy limitof the employed data, early-type Be stars show more frequentoutbursts (mean outburst rate of N ob = 2.3 ± . yr − ) than mid-( N ob = 0.7 ± . yr − ) and late-type objects ( N ob = 0.2 ± . yr − ). • On the other hand, we cannot confirm the finding of LB17that outbursts have a higher occurrence rate in early-type stars thanin mid- and late-type objects. This is likely a result of their datasource’s bias against objects with rare outbursts. No statisticallysignificant trend is seen in the results for the ASAS sample, and theresulting distribution is essentially flat. Outbursts, therefore, are acommon characteristic of Be stars of all subtypes. • Our results indicate that the mean amplitude of outbursts de-creases from early-type through late-type Be stars. • We have measured rising and falling times for well-covered andwell-defined outbursts in our sample stars and confirm that nearlyall outburst events are characterized by falling times that exceedthe rising times (median rising time of 28.5 d; median falling timeof 51.0 d). No differences were found between early-, mid- andlate-type stars. Instead, we find that a single non-linear functionadequately describes the ratio of falling time to rising time acrossall spectral subtypes, with the ratio being larger for short events.
ACKNOWLEDGEMENTS
We thank our referee, Dr. Dietrich Baade, for his thoughtful and de-tailed report which helped to greatly improve the paper. Guoshou-jing Telescope (the Large Sky Area Multi-Object Fiber Spectro-scopic Telescope LAMOST) is a National Major Scientific Projectbuilt by the Chinese Academy of Sciences. Funding for the projecthas been provided by the National Development and Reform Com-mission. LAMOST is operated and managed by the National As-tronomical Observatories, Chinese Academy of Sciences. This re-search has made use of the SIMBAD database and the VizieRcatalogue access tool, operated at CDS, Strasbourg, France, andthe AAVSO Photometric All-Sky Survey (APASS), funded by theRobert Martin Ayers Sciences Fund.
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APPENDIX A: ESSENTIAL DATA
MNRAS000
MNRAS000 , 1–46 (2017) n i n ve s ti ga ti ono ft h e pho t o m e t r i cv a r i ab ilit y o f c onfi r m e dand c and i da t e G a l a c ti c B e s t a rs u s i ng A S A S - t a Table A1Essential data for our sample stars, sorted by increasing right ascension. The columns denote: (1) Internal identification number. Stars were numbered in order of increasing rightascension. (2) Identification from the Guide Star Catalog (GSC), version 1.2. (3) Identification from the Henry Draper (HD) catalogue or other conventional identifier. (4) Right ascension(J2000; Høg et al. 2000). (5) Declination (J2000; Høg et al. 2000). (6) V magnitude range, as derived from ASAS-3 data. Ranges that have been corrected for light contamination from closeneighbouring stars (cf. Section 2.5) are marked by an asterisk. (7) V magnitude range, as gleaned from a star’s recorded photometric history (cf. Section 2.5). (8) Spectral type from theliterature. (9) Subtype (E=early; M=mid; L=late; U=unclassified). (10) Emission flag (emission confirmed: l=in literature/BeSS spectra; s=in own spectra; la=in LAMOST spectra; u=from uvby β photometry). (11) variability type, following LB17: ObV=outbursts present; SRO=semi-regular outbursts; LTV=long-term variability present; NRP=non-radial pulsator candidate(periodic variability with P ≤ d); IP=intermediate periodicity (periodic variability with < P ≤ d); EB=eclipsing binary. (12) variability type, following the GCVS and VSXclassifications. (13) variability period(s), as derived from analysis of ASAS-3 data. (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)No. IDGSC IDalt α (J2000) δ (J2000) Range( V ) Range( V ) Spec.type subtype emission Var.type Var.type Period(s)[mag] lit.[mag] lit. [E/M/L/U] flag [LB17] [GCVS/VSX] [d]1 GSC06464-00405 HD29557,NSV16132 043816.174 -243930.77 8.48-8.63 8.45-8.64 B5Ib/IIp:shell?(Houk&Smith-Moore1988b),B3Ve(Levenhagen&Leister2006) M l ObV GCAS2 GSC01845-02192 HD32318,NSV16230 050317.288 +234917.46 8.39-8.63 8.38-8.63 B3IV(Straižysetal.2003),A2e(McCarthy&Treanor1965) U l ObV GCAS3 GSC08877-00138 HD33599,NSV16255 050712.946 -614818.31 8.79-9.20 8.79-9.20 B2Vep(Levenhagen&Leister2006),B5pshell(Houk&Cowley1975) M l,u ObV,NRP GCAS+LERI 1.10487(9)4 GSC04755-00818 HD293881,ASASJ051449-0310.0 051449.040 -030959.06 11.30-11.58* 11.30-11.58 B9(Cannon&Mayall1949),em(Wiramihardjaetal.1991) L l LTV GCAS5 GSC09162-00751 HD269649,ASASJ053022-6919.7 053022.553 -691938.95 10.41-10.81* 10.41-10.81 em(Howarth2012),B2.5:(Rousseauetal.1978) E l SRO GCAS6 GSC00115-01423 HD37330,NSV2478 053753.455 +005806.98 7.30-7.47 7.30-7.49 B6Vne(Warren&Hesser1978) M l,u LTV,NRP GCAS+LERI 0.77143(5)7 GSC01310-01587 HD37901,ASASJ054240+2134.7 054239.812 +213443.29 8.95-9.08 8.95-9.08 A0II/III(Hardorpetal.1965) L LTV GCAS8 GSC01311-01238 HD38191,ASASJ054456+2127.6 054456.235 +212738.48 8.42-8.74 8.42-8.74 B1:V:ne:(Morganetal.1955) E l ObV,LTV GCAS9 GSC06491-00717 HD40193,SAO171041 055622.484 -223900.05 9.15-9.30* 9.14-9.30 B8Vne:(Houk&Smith-Moore1988b),Be(Bidelman&MacConnell1973) L l ObV GCAS10 GSC01868-01264 BD+251081,ASASJ060149+2537.9 060149.500 +253752.73 10.34-10.44 10.23-10.44 OB-(McCuskey1967) U LTV GCAS11 GSC00721-02056 HD250980,ASASJ060334+0939.9 060334.246 +093954.65 9.45-9.58 9.45-9.58 Be(Bidelman&MacConnell1973),B2ne(Popper1950) E l LTV GCAS12 GSC01864-00314 ALS8684,ASASJ060445+2324.1 060445.296 +232407.25 11.25-11.57 11.25-11.57 OB(McCuskey1967) U la ObV GCAS13 GSC00738-01213 ASASJ060954+1300.3 060953.686 +130012.93 11.20-11.72 11.20-11.72 OB:e(Stephenson&Sanduleak1977a),binary U l,la SRO GCAS 360(5)14 GSC00742-01475 ASASJ061353+1418.0 061352.522 +141802.15 10.89-11.24 10.89-11.24 pec(McCuskey1959) U ObV GCAS15 GSC00739-01143 BD+111084,ASAS061535+1125.9 061535.038 +112552.86 10.27-10.50 10.27-10.54 OBe(Nassauetal.1965) U l,la ObV GCAS16 GSC00739-01342 HD254329,ASASJ061624+1223.8 061624.004 +122350.06 9.20-9.50 9.20-9.50 OBe(Nassauetal.1965),B8e(Merrill&Burwell1943) L l ObV GCAS17 GSC01319-00734 HD255103,ASASJ061940+1822.3 061939.964 +182217.30 10.49-10.84 10.48-10.84 OB+e(Stephenson&Sanduleak1971) U l ObV GCAS18 GSC00743-02467 HD44351,ASASJ062159+1418.5 062158.770 +141832.26 8.22-8.53 8.22-8.53 B8Ib/II(Nassauetal.1965),B3eshell(Merrill&Burwell1949) L l LTV GCAS19 GSC00732-02105 HD256577,ASASJ062400+0818.0 062400.179 +081802.49 9.48-9.78 9.31-9.78 B1V(Turner1976),B2IV:e:p(Hiltner1956) E l,u SRO GCAS20 GSC00154-02436 HD259481,ASASJ063259+0456.4 063259.376 +045622.50 9.41-9.68* 9.35-9.68 B0Ve(Vranckenetal.1997) E l,la ObV GCAS21 GSC00733-01509 HD259631,ASASJ063343+0802.1 063343.417 +080210.00 9.51-9.57 9.51-9.59 B1Vnne(Turner1976) E l,u LTV BE22 GSC00733-01932 HD260360,ASASJ063551+0756.4 063551.182 +075624.56 10.85-11.07 10.77-11.07 B3III(Voroshilovetal.1985),em(Skiff2014) E l ObV GCAS23 GSC00146-01543 HD288847,ASASJ063627+0140.4 063627.868 +014021.28 9.56-9.87 9.56-9.87 B5(Skiff2014),em(Merrill&Burwell1950) M l ObV GCAS24 GSC00154-00165 HD260765,ASASJ063707+0535.0 063706.595 +053457.99 10.27-10.49 10.16-10.49 B8III(Voroshilovetal.1985) L LTV GCAS25 GSC00755-00857 ASASJ064801+1300.2 064801.247 +130013.03 11.59-11.97 11.59-11.99 OB:e(Stephenson&Sanduleak1977b) U l,la ObV GCAS26 GSC00152-00780 ASASJ064839+0205.3 064839.065 +020520.06 11.53-12.04* 11.53-12.05 em(Robertson&Jordan1989) U l SRO GCAS27 GSC00148-02601 HD292379,ASASJ064926+0035.0 064925.983 +003500.07 10.02-10.13* 9.98-10.13 em(MacConnell1981),OB-(Nassauetal.1965) U l LTV BE28 GSC00160-01058 HD264600,ASASJ064937+0613.6 064936.772 +061332.34 10.82-11.05 10.80-11.19 B2Vnne(Vijapurkar&Drilling1993) E l SRO GCAS 259(5)29 GSC05387-01121 HD49888,NSV3231 065008.089 -123505.12 7.22-7.50 7.18-7.50 em(Bidelman1988),B5e(Neubauer1943),B5Iab/Ib(Houk&Smith-Moore1988b) M l,u LTV GCAS30 GSC04801-00017 ASASJ065244-0011.3 065244.027 -001116.77 11.26-11.55 11.13-11.55 B:(McCuskey1956),em(Robertson&Jordan1989) U l ObV GCAS31 GSC05383-00187 HD50424,SAO133821 065253.052 -100026.93 8.79-8.92 8.79-8.98 B8e(Stephenson&Sanduleak1977a) L l,u LTV GCAS32 GSC04805-00043 HD50891,ASASJ065459-0342.0 065458.824 -034201.29 8.76-9.09 8.76-9.09 B1IIIe(Negueruelaetal.2004),B0:ep(Morganetal.1955),B0.5Ve(Chojnowskietal.2015) E l,s SRO,LTV GCAS33 GSC05388-01118 BD-121700,ASASJ065555-1300.0 065555.052 -130001.82 10.47-10.93 10.47-10.93 OBe(Stephenson&Sanduleak1971),em(Merrill&Burwell1950) U l SRO GCAS34 GSC00748-01908 HD267003,ASASJ065729+0759.3 065728.901 +075920.05 11.12-11.34 11.09-11.34 Be(Stephenson&Sanduleak1977b) U l,la ObV GCAS35 GSC04809-00545 HD295852,ASAS065752-0345.8 065751.546 -034546.65 9.28-9.58 9.28-9.63 Be(Bidelman&MacConnell1973),B3e(Münch1952) E l ObV,LTV GCAS36 GSC00153-00891 ASASJ065831+0259.1 065831.540 +025905.46 12.35-12.78 12.35-12.78 em(Stephenson&Sanduleak1977b) U l SRO GCAS37 GSC04801-01915 ASASJ065910-0037.2 065909.981 -003710.55 11.14-11.33 11.14-11.35 em(Robertson&Jordan1989),B5(McCuskey1956) M l ObV GCAS38 GSC04826-00257 ASASJ070241-0709.5 070241.275 -070932.72 10.98-11.18* 10.82-11.18 em(MacConnell1981) U l LTV GCAS39 GSC04826-01079 ASASJ070334-0712.4 070334.270 -071227.79 11.17-11.41 11.17-11.41 em(MacConnell1981) U l ObV GCAS40 GSC05393-02168 BD-131825,ASASJ070658-1340.6 070658.226 -134035.18 9.17-9.65 9.17-9.65 Be(Bidelman&MacConnell1973) U l,u SRO GCAS41 GSC05968-03899 HD54576,SAO152454 070837.741 -173805.02 9.44-9.53* 9.44-9.55 B7/8II,(Anderson&Francis2012) L ObV GCAS42 GSC05398-01016 HD55439,ASASJ071235-0950.7 071234.812 -095042.09 8.29-8.52 8.29-8.52 B2Ve(Claria1974) E l,u,s LTV,ObV GCAS43 GSC05973-00249 NSV17397,BD-201805 071458.243 -203712.21 10.27-10.66* 10.27-10.67 B2IIIne(Vijapurkar&Drilling1993) E l ObV,LTV GCAS44 GSC05399-00962 HD56873,NSV3525 071830.832 -103520.15 10.52-10.74 10.51-10.78 B8e:(Stephenson&Sanduleak1977b) L l ObV GCAS45 GSC07634-01561 HD57551,ASASJ071959-4029.7 071959.383 -402941.60 9.68-9.90 9.68-9.90 em(Henize1976),B8III(Houk1978) L l ObV GCAS46 GSC04820-02947 ASASJ072024-0337.7 072024.300 -033738.72 10.26-10.40 10.26-10.41 B7e(Stephenson&Sanduleak1977a) L l ObV GCAS47 GSC05978-01855 BD-201891 072236.249 -205434.82 9.45-9.66 9.45-9.66 Be,(Stephenson&Sanduleak1977a),B2.5Vne(Garrisonetal.1977) E l ObV GCAS48 GSC05978-00030 ASASJ072628-2205.2 072628.027 -220513.78 11.78-12.31* 11.78-12.31 em(MacConnell1981) U l SRO GCAS 1560(50)49 GSC05983-00995 HD59479,GDS_J0729316-173620 072931.668 -173620.68 9.89-10.06 9.83-10.06 B5V(Münch1952) M ObV,LTV GCAS50 GSC07109-00828 CPD-321553,ASASJ073300-3233.2 073300.270 -323311.05 10.47-10.69 10.47-10.69 Be(Bidelman&MacConnell1973) U l LTV GCAS51 GSC05405-00431 HD60993,NSV17524 073642.296 -130349.89 8.86-8.98 8.70-8.98 B3n(Neubauer1943) E u LTV GCAS52 GSC05988-00265 NSV17539,BD-181948 073924.704 -184832.93 10.33-10.46 10.30-10.69 OB+e(Stephenson&Sanduleak1971) U l LTV BE53 GSC08552-00688 HD62483,NSV17565 074128.928 -531141.14 8.06-8.25 8.06-8.27 B2III(Hill1970),B2II(Houk1978) E u SRO GCAS54 GSC06552-00580 ASASJ074314-2829.2 074313.945 -282912.94 12.12-12.80 12.12-12.80 OB+(Orsatti1992),em(Henize1976) U l SRO GCAS: 269(9)55 GSC06552-01189 CD-294913,ASASJ074559-2933.2 074559.001 -293316.13 11.05-11.46 11.05-11.53 OB+e(Orsatti1992) U l LTV GCAS56 GSC07106-02534 CD-305070,ASASJ074630-3115.6 074630.000 -311532.05 11.13-11.43* 11.13-11.54 OBe(Orsatti1992) U l SRO GCAS 720(20)57 GSC07123-00519 CD-334170,ASASJ074829-3324.2 074829.103 -332410.14 11.74-12.05* 11.69-12.06 OB+e(Orsatti1992) U l ObV,SRO: GCAS58 GSC08135-03248 HD64596,ASASJ075233-4628.5 075233.235 -462830.09 9.15-9.53 9.15-9.53 B2V(Houk1978) E SRO,EB EA+GCAS 1.28212(1)59 GSC06565-01179 NSV17662,CPD-292176 075542.491 -293353.56 10.37-10.95 10.22-10.98 B0V(n)e(Vijapurkar&Drilling1993),B0Ve(Fernieetal.1966) E l ObV GCAS60 GSC07124-01160 ALS913,ASASJ075930-3204.7 075930.375 -320438.75 11.82-12.47* 11.82-12.47 OB+e(Orsatti1992) U l SRO GCAS 291(4)61 GSC07120-02077 NSV17698,CPD-302160 075943.672 -304126.35 10.59-11.05* 10.59-11.05 B1IIInne(Vijapurkar&Drilling1993) E l SRO GCAS62 GSC06562-00688 HD67123,ASASJ080533-2740.5 080532.896 -274020.40 9.99-10.26 9.99-10.26 Be(Stephenson&Sanduleak1977b),A3(Cannon&Pickering1919a) U l ObV GCAS63 GSC05421-00568 ASASJ080723-1247.1 080723.294 -124706.71 11.22-11.62 11.22-11.62 em(MacConnell1981) U l ObV GCAS64 GSC07659-01614 CD-384113,ASASJ080845-3857.5 080844.976 -385735.13 11.17-11.40* 11.17-11.44 em(MacConnell1981) U l ObV GCAS M N R A S , ( ) B e r nha r d e t a l . Table A1continued. (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)No. IDGSC IDalt α (J2000) δ (J2000) Range( V ) Range( V ) Spec.type subtype emission Var.type Var.type Period(s)[mag] lit.[mag] lit. [E/M/L/U] flag [LB17] [GCVS/VSX] [d]65 GSC05438-00850 HD68468,NSV17783 081200.394 -141008.35 8.67-8.82 8.67-8.82 Bshell,(Bidelman&MacConnell1973),B3:eshell,(Guetter1968) E l,s,u ObV,LTV GCAS66 GSC07125-02097 NSV17791,CPD-322038 081212.588 -322815.06 10.99-11.36* 10.75-11.37 B0IIIe(Boschetal.2003) E l SRO GCAS67 GSC05435-00526 HD71072,NSV17879 082500.396 -124553.24 6.87-6.94 6.87-6.94 B7IVe(Buscombe1969) L l LTV,NRP BE 1.09207(8)68 GSC07669-01154 USNO-A2.00450-06879300 082802.327 -414457.16 12.18-12.41 12.17-12.41 U ObV GCAS69 GSC07669-03714 HD72014,NSV17900 082852.061 -423514.91 6.23-6.68 6.20-6.68 B1III(Cucchiaroetal.1980),B0V:nne,(Garrisonetal.1977),B1/2V:nne(Houk1978) E l,s,u ObV GCAS70 GSC07139-02209 HD71964,SAO199281 082901.345 -332739.42 8.81-8.90* 8.76-8-90 A0III/IV(Houk1982) L LTV GCAS:71 GSC08151-01868 CPD-452826,GDS_J0840509-460545 084050.921 -460545.36 9.91-10.30* 9.91-10.30 B2Vne(Fitzgeraldetal.1979),B2:Vne(Feastetal.1961) E l ObV GCAS72 GSC08155-02404 HD74401,ASASJ084200-4739.9 084200.380 -473953.92 8.90-8.99 8.90-9.02 B1.5IIIne(Garrisonetal.1977) E l LTV BE73 GSC08164-01530 HD76568,SAO236395 085457.808 -505150.36 9.39-9.51 9.39-9.51 B1V:nne(Houk1978),B7e(Stephenson&Sanduleak1977a) M l ObV GCAS74 GSC08594-00620 HD77032,ASASJ085715-5835.2 085715.412 -583509.68 8.67-8.80 8.67-8.80 B2:Vne(Garrisonetal.1977),B5Vne(Houk&Cowley1975) M l,s,u ObV GCAS75 GSC08165-00324 CD-464821,ASASJ090014-4641.1 090014.047 -464108.57 8.95-9.06 8.95-9.06 B2Vn(Slawson&Reed1988),Be(Stephenson&Sanduleak1977a) E l LTV BE76 GSC08582-02609 HD299794,ASASJ090036-5321.0 090036.167 -532102.25 9.78-9.98 9.78-9.98 em(Henize1976),OB(Stephenson&Sanduleak1971) U l LTV,IP BE 25.80(4)77 GSC08591-00039 HD302105,SAO236686 091036.634 -573148.79 9.46-9.63* 9.46-9.63 B(Stephenson&Sanduleak1977a),em(Henize1976),B1IVn(Garrisonetal.1977) E l LTV BE78 GSC07686-01898 CPD-413411,ASASJ091049-4228.6 091049.165 -422837.91 10.11-10.24* 10.11-10.24 B7e(Herbst1975) L l ObV GCAS79 GSC08587-02162 HD79778,ASASJ091351-5532.4 091351.368 -553222.77 8.06-8.46* 8.06-8.46 B2IVne(Garrisonetal.1977) E l,s,u SRO GCAS80 GSC08174-00235 HD298335,ASASJ092111-5030.8 092110.586 -503044.92 10.15-10.53* 10.15-10.53 B7e(Stephenson&Sanduleak1977a),B2/4(Sundmanetal.1974),B5II/Ib(Kennedy1996) U l ObV GCAS81 GSC09196-00424 NSV4471 092111.015 -683947.93 11.65-11.82 11.65-11.82 U LTV,NRP LERI+BE 1.14514(10)82 GSC08588-02569 HD81354,ASASJ092255-5544.2 092254.755 -554411.97 9.14-9.37* 9.14-9.37 B3/5Ve(Houk&Cowley1975) M l,u ObV GCAS83 GSC08167-01520 HD82830,ASASJ093309-4645.9 093309.092 -464554.48 9.21-9.39 9.20-9.39 B0/2Ie(Houk1978),Be(Bidelman&MacConnell1973),B1III:ne(Garrisonetal.1977) E l,u LTV,ObV GCAS84 GSC08593-01904 HD83060,NSV18234 093342.391 -570948.09 9.07-9.14* 9.07-9.14 Be(Stephenson&Sanduleak1977a),B2Vnne(Houk&Cowley1975),B2IV-Vnep(shell)(Garrisonetal.1977) E l LTV,NRP LERI 0.73486(1)85 GSC08585-02212 HD83597,ASASJ093751-5340.9 093750.894 -534049.23 9.08-9.34 9.08-9.34 B1.5Ve(Garrisonetal.1977) E l,s,u ObV,LTV GCAS86 GSC08593-00336 HD83781,SAO237182 093843.500 -564821.06 9.46-9.73 9.46-9.73 B8/9V(Houk&Cowley1975) L ObV GCAS87 GSC07179-02573 HD83739 093933.173 -364031.89 9.89-10.10 9.89-10.10 em(Henize1976),B8(Cannon&Pickering1919b) L l LTV GCAS88 GSC08593-02269 HD84361 094242.693 -580619.69 8.17-8.43* 8.17-8.43 em(Henize1976),B2/3V(Houk&Cowley1975) E l,u ObV,LTV,IP GCAS+LERI: 4.62256(9)89 GSC08606-00053 HD85495,GDS_J0950146-580245 095014.687 -580245.12 7.90-8.06 7.90-8.06 em(Henize1976),B4II/III(Houk&Cowley1975),B5(Lodenetal.1976) M l,s LTV GCAS90 GSC08598-02245 HD85809,ASASJ095238-5419.1 095238.445 -541907.59 9.07-9.42* 9.07-9.47 B2/3III/V(Houk&Cowley1975) E SRO GCAS 120.5(8)91 GSC08606-02020 CPD-562606,ASASJ095308-5636.5 095307.478 -563629.24 10.30-10.81 10.29-10.81 em(Henize1976),OB+e(Stephenson&Sanduleak1971) U l SRO GCAS92 GSC08610-03102 HD86657,ASASJ095758-5957.6 095758.374 -595737.45 9.66-9.79* 9.66-9.79 B5(Gieseking1980) M ObV,LTV GCAS93 GSC08603-00164 HD300425,ASASJ100139-5500.8 100139.127 -550046.36 9.78-10.10 9.78-10.10 em(MacConnell1981),OBe(Stephenson&Sanduleak1971) U l SRO GCAS 152(4)94 GSC08599-02357 HD87203,ASASJ100152-5412.4 100152.354 -541221.12 8.50-8.75 8.50-8.75 Be(Stephenson&Sanduleak1977a),B5Ve(Houk&Cowley1975),O9.5/B1(Nordström1975) M l,s,u ObV GCAS95 GSC08611-01377 HD87565 100350.777 -595123.35 9.30-9.66* 9.30-9.66 B2Ve(González&Lapasset2001),B2Vnne(Levato&Malaroda1975) E l,u ObV GCAS96 GSC08603-00677 CPD-543090,ASAS100446-5517.5 100446.026 -551730.05 11.05-11.40 11.05-11.40 B7e(Stephenson&Sanduleak1977a),B2/4(Nordström1975) M l ObV GCAS97 GSC08955-00160 HD87849 100510.339 -671530.81 8.94-9.07* 8.94-9.07 B4V(Houk&Cowley1975) M ObV GCAS98 GSC08943-00584 HD304915 100636.154 -604906.70 10.12-10.39* 10.12-10.45 em(MacConnell1981),B5V(Lodenetal.1976) M l ObV GCAS99 GSC08607-01004 Hen3-375,ASASJ101045-5620.0 101045.371 -562001.71 12.09-12.57 12.09-12.57 OB+:e(Stephenson&Sanduleak1977a) U l SRO GCAS100 GSC08607-00285 HD300584,NSV18347 101059.296 -570926.44 10.08-10.28 10.08-10.29 O5/B0e(Lodenetal.1976),B1Ve(Graham1970) E l ObV GCAS101 GSC08604-00356 HD300540,Hen3-388 101331.708 -545359.40 9.81-9.93* 9.81-9.93 em(Henize1976),B6/7(Lodenetal.1976) M l LTV,ObV GCAS102 GSC08947-00809 NSV18363,CPD-621480 101335.005 -630011.72 11.11-11.27 10.82-11.27 em(Henize1976),OB+e(Stephenson&Sanduleak1971) U l ObV GCAS103 GSC08943-02244 HD305019,NSV18365 101502.400 -605521.23 10.17-10.55* 10.17-10.57 Oem(Lodenetal.1976),B0ep(Humphreys1973) E l ObV GCAS104 GSC08943-00620 ALS1476,ASASJ101605-6032.8 101604.411 -603252.25 11.32-11.85* 11.32-11.85 B2III(Vijapurkar&Drilling1993),OB+(Stephenson&Sanduleak1971) E LTV,ObV GCAS105 GSC08612-00975 GDS_J1019327-582544 101932.785 -582543.73 11.82-12.19* 11.82-12.19 B:e(Stephenson&Sanduleak1977a) U l ObV GCAS106 GSC08608-00434 HD300683 101936.677 -570738.11 9.68-9.94 9.68-9.94 Bshell(Bidelman&MacConnell1982),B3/6(Lodenetal.1976) M l ObV GCAS107 GSC08608-00807 HD89990 102136.561 -575552.81 9.70-9.78* 9.70-9.79 B8(Lodenetal.1976),B8V(Houk&Cowley1975) L ObV GCAS108 GSC08608-00914 HD90187,NSV18395 102307.843 -575951.23 8.67-9.08* 8.65-9.08 B1IIne(Turner1978),B1IIIne(Garrisonetal.1977) E l,s,u SRO GCAS109 GSC08612-00331 HD302816,CPD-582166 102426.028 -592423.88 9.81-10.16* 9.81-10.16 B2V(Lodenetal.1976) E ObV GCAS110 GSC08608-02412 HD90551 102550.913 -563715.23 8.60-8.73* 8.55-8.77 em(Henize1976),B3Vn(e?)(Houk&Cowley1975) E l,s LTV GCAS111 GSC08612-00380 HD302798,ASASJ102559-5859.7 102558.956 -585944.69 9.86-10.28* 9.86-10.32 B3V(e)(Graham1970),em(Henize1976) E l SRO GCAS112 GSC08608-00239 HD300739,ASASJ102609-5712.1 102609.450 -571206.70 10.21-10.46* 10.21-10.46 em(MacConnell1981),O9.5/B0(Lodenetal.1976) E l SRO GCAS113 GSC09397-00615 HD91180,ASASJ102758-7613.9 102758.238 -761356.84 9.09-9.20* 9.09-9.20 em(Henize1976),B5:e(Houk&Cowley1975) M l ObV GCAS114 GSC08609-01016 HD302838,NSV18417 102831.527 -574218.23 9.94-10.31* 9.87-10.31 OB:e(Lodenetal.1976),B1Vne(Graham1970) E l ObV GCAS115 GSC08605-01985 CPD-543736,ASAS102934-5508.2 102934.257 -550810.17 10.72-10.84* 10.72-10.84 Be(Stephenson&Sanduleak1977b),B5(Lodenetal.1976) M l LTV,ObV GCAS116 GSC08956-01223 HD91597,NSV18440 103301.134 -605041.77 9.54-9.95* 9.54-9.95 B1IIIn(e)(Garrisonetal.1977),B7/8IV/V(Houk&Cowley1975) M l SRO GCAS117 GSC08613-01412 HD302977,CPD-573419 103308.321 -582607.90 10.07-10.25 10.07-10.25 B0(Sundmanetal.1974),em(Wray1966),A(Nesterovetal.1995) E l ObV GCAS118 GSC08613-00130 HD302978,CPD-573422 103309.422 -582840.93 8.74-8.81* 8.74-8.81 B5(Nesterovetal.1995) M LTV BE:119 GSC08613-01744 WRAY15-604,ASASJ103323-5831.8 103322.896 -583150.08 11.76-12.41 11.76-12.41 OB+:e(Stephenson&Sanduleak1977a) U l ObV GCAS120 GSC08613-00147 CPD-582312,GDS_J1034088-592853 103408.845 -592854.01 10.27-10.84* 10.27-10.84 em(Henize1976),Be(Bidelman&MacConnell1973) U l SRO GCAS121 GSC08957-02248 HD92064 103619.681 -603729.81 10.03-10.28* 10.03-10.28 em(MacConnell1981),B3/6V:(Houk&Cowley1975) M l ObV GCAS122 GSC08609-00597 HD303147,CPD-573618 103835.398 -575334.17 9.95-10.22* 9.95-10.22 B3(Nesterovetal.1995),B1/3(Sundmanetal.1974) E ObV GCAS123 GSC08622-01179 HD303142,CPD-563632 104000.582 -573259.21 9.58-9.94* 9.53-9.94 em(MacConnell1981),OB(Stephenson&Sanduleak1971) U l ObV,NRP GCAS+LERI 0.483815(7)124 GSC08622-00429 HD92759,ASASJ104121-5739.9 104121.316 -573951.47 9.39-9.84* 9.39-9.84 em(Schwartzetal.1990),B2Ve(Graham1970) E l SRO GCAS125 GSC08626-00271 HD303190,GDS_J1041231-590918 104123.163 -590918.81 10.12-10.23* 10.12-10.26 B1V(Fitzgerald&Mehta1987),B2V(Forte&Orsatti1981) E LTV BE126 GSC08957-03483 CPD-611814 104218.409 -614523.99 11.29-11.62* 11.29-11.62 U ObV GCAS127 GSC08961-01212 Hen3-476,2MASS10424993-6159377 104249.948 -615937.73 11.84-12.22* 11.79-12.22 B2:,(Sundmanetal.1974);em(Henize1976) E l LTV BE128 GSC08618-01375 HD93051 104335.610 -555542.22 9.73-9.83* 9.73-9.83 B8/9III(Houk&Cowley1975) L ObV GCAS M N R A S , ( ) n i n ve s ti ga ti ono ft h e pho t o m e t r i cv a r i ab ilit y o f c onfi r m e dand c and i da t e G a l a c ti c B e s t a rs u s i ng A S A S - t a Table A1continued. (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)No. IDGSC IDalt α (J2000) δ (J2000) Range( V ) Range( V ) Spec.type subtype emission Var.type Var.type Period(s)[mag] lit.[mag] lit. [E/M/L/U] flag [LB17] [GCVS/VSX] [d]129 GSC08622-01758 HD93442,NSV18520 104606.001 -564525.47 8.77-8.93* 8.77-8.93 B3(Cannon&Mayall1949),em(Henize1976) E l ObV GCAS130 GSC08622-01002 HD303333,CPD-563785 104621.227 -573732.19 11.14-11.27* 11.13-11.28 A2(Nesterovetal.1995) U LTV GCAS131 GSC08618-01665 HD93561,NSV18527 104659.466 -544952.60 8.86-9.38* 8.86-9.38 B1III:nne(Garrisonetal.1977),B1/3e(Houk&Cowley1975) E l,u SRO GCAS132 GSC08622-01017 HD93618,ASASJ104722-5710.0 104722.142 -571001.93 9.01-9.19* 9.01-9.19 OB(Stephenson&Sanduleak1971),B2Ve(Graham1970) E l,u LTV,NRP BE+LERI 0.88286(2)133 GSC08965-01363 HD308023,CPD-631673 104800.558 -643149.40 9.95-10.10* 9.94-10.10 OB-e(Stephenson&Sanduleak1971),B3IVe(Graham1970) E l LTV GCAS134 GSC08969-00788 HD310250,CPD-651515 104824.521 -662341.64 9.92-10.19* 9.92-10.19 em(Henize1976) U l ObV GCAS135 GSC08958-02421 HD94288,GDS_J1051408-614136 105140.876 -614136.09 9.20-9.54* 9.20-9.55 em(Henize1976),B3/5V(Houk&Cowley1975) M l,u SRO GCAS136 GSC08623-02851 CPD-553970 105457.445 -563943.55 11.38-11.52* 11.38-11.54 em(MacConnell1981) U l ObV GCAS137 GSC08958-02242 HD305829,GDS_J1056461-614635 105646.201 -614635.31 10.22-10.48 10.15-10.48 U SRO GCAS138 GSC08619-01981 HD301197,CPD-544219 105918.999 -552934.25 9.71-9.90* 9.63-9.90 em(Henize1976) U l LTV,NRP BE+LERI: 0.2356186(10)139 GSC08627-00455 HD303669,CPD-582933 110050.878 -585948.33 9.43-9.58* 9.43-9.58 OB(Graham&Lynga1965),B5(Wallenquist1931) M LTV,NRP BE+LERI:140 GSC08627-01249 HD95615,GDS_J1101143-590900 110114.361 -590900.62 9.12-9.31* 9.11-9.40 B3II/III(Houk&Cowley1975),B2V(Humphreys1973) E SRO GCAS141 GSC08958-02961 HD95826A,ASASJ110223-6030.9 110223.915 -603058.51 9.21-9.36* 9.10-9.36 B5e(Cannon&Pickering1919b),em(Henize1976),Be(Bidelman&MacConnell1973) M l LTV,IP BE 23.0(2)142 GSC08627-02220 HD303763,CPD-582969 110250.868 -591905.90 10.10-10.27* 10.09-10.27 em(Henize1976),Be(Bidelman&MacConnell1973) U l ObV GCAS143 GSC08958-03515 CPD-592978,GDS_J1102595-602911 110259.577 -602911.24 10.70-10.95 10.63-10.95 em(Henize1976) U l LTV GCAS144 GSC08627-02146 HD303764,GDS_J1103042-592218 110304.300 -592218.72 10.82-11.00 10.82-11.04 A(Wallenquist1931) L ObV GCAS145 GSC08958-00887 HD95972,ASASJ110310-6146.1 110309.683 -614607.53 8.64-9.00* 8.64-9.02 B2Vnn(Houk&Cowley1975),B2Ve(Graham1970) E l,u ObV GCAS146 GSC08958-01376 HD96447,CPD-602517 110600.796 -611033.95 8.94-9.20* 8.94-9.20 B3(Loden1980),B2/3V:(Houk&Cowley1975),B9V(Martin1964) M u LTV BE147 GSC08958-03463 Hen3-575,2MASS11061965-6046352 110619.672 -604635.25 11.56-11.74* 11.56-11.74 B5e(Stephenson&Sanduleak1977a) M l LTV GCAS148 GSC08958-03384 HD306093,GDS_J1108184-604801 110818.423 -604801.10 10.71-11.00* 10.71-11.05 B8(Nesterovetal.1995),B1/3(Sundmanetal.1974) U ObV GCAS149 GSC08959-00482 HD306111 110919.827 -610605.36 10.09-10.26* 10.08-10.26 em(Henize1976),Be(Bidelman&MacConnell1973),B2Ve(Graham1970) E l ObV GCAS150 GSC08967-00393 HD97136 110948.048 -634739.30 9.16-9.30* 9.16-9.30 B2III(Garrisonetal.1977) E SRO GCAS151 GSC08959-00488 HD306082,GDS_J1109573-604622 110957.356 -604623.00 9.81-10.09* 9.81-10.09 B0(Johansson1980),B5e(Stephenson&Sanduleak1977a) E l,u ObV GCAS152 GSC08628-00661 HD303887,ASASJ111052-5813.0 111052.287 -581301.86 9.27-9.64* 9.27-9.64 B5e(Stephenson&Sanduleak1977a) M l ObV GCAS153 GSC08959-00863 HD306205 111329.502 -611550.95 9.87-10.15* 9.87-10.15 Be(Stephenson&Sanduleak1977a),B1.5Vne(Feastetal.1961) E l SRO GCAS154 GSC08959-00846 HD306209,GDS_J1113347-612042 111334.727 -612042.84 9.86-10.14* 9.86-10.16 B1Ve(Graham1970) E l ObV GCAS155 GSC08620-01856 HD97792 111420.001 -560251.23 7.89-8.04* 7.86-8.04 B7e(Stephenson&Sanduleak1977a) L l,s ObV GCAS156 GSC08959-02476 HD306196 111429.446 -610321.45 9.52-9.75* 9.52-9.75 em(MacConnell1981),B0:Vn(Feastetal.1961),O9.5V(Martin1964) E l ObV GCAS157 GSC08625-00369 HD304395 113108.510 -571451.12 9.30-9.38* 9.25-9.38 B7e(Stephenson&Sanduleak1977a) L l LTV BE158 GSC08980-01582 NSV18793,ALS2385 113306.654 -644201.88 11.34-11.83* 11.33-11.83 em(Henize1976),OB+e(Stephenson&Sanduleak1971) U l ObV,LTV GCAS159 GSC08972-00064 HD306657,NSV18800 113515.172 -614159.57 10.36-10.54* 10.36-10.54 em(Henize1976),OBe(Stephenson&Sanduleak1971) U l,u ObV GCAS160 GSC08972-00932 HD101221 113821.470 -603739.76 9.20-9.44* 9.20-9.44 B9(Cannon&Pickering1919b) L u ObV GCAS161 GSC08642-01087 HD306958,GDS_J1140458-595946 114045.061 -595946.93 10.35-10.57* 10.35-10.57 em(Henize1976) U l ObV GCAS162 GSC08973-00795 HD307007,ASASJ114322-6111.3 114321.298 -611121.18 9.91-10.11* 9.91-10.11 em(Henize1976),OB-:e(Stephenson&Sanduleak1971) U l LTV BE163 GSC08973-00729 HD309065 114545.780 -612752.77 8.72-8.84* 8.72-8.84 B:e(Stephenson&Sanduleak1977a) U l,u LTV BE164 GSC08985-01836 CPD-651722,ASASJ114755-6614.7 114754.897 -661441.53 11.19-11.48 11.19-11.48 Be(Stephenson&Sanduleak1977a) U l ObV GCAS165 GSC08639-01611 HD102564,ASASJ114805-5726.0 114805.120 -572602.30 8.66-8.95* 8.66-8.95 B2III(Houk&Cowley1975) E s SRO GCAS166 GSC08643-01679 HD307293,GDS_J1151597-595906 115159.696 -595907.12 9.85-10.10* 9.85-10.10 em(Henize1976),OBe(Stephenson&Sanduleak1971),B3(Bourgésetal.2014) E l ObV GCAS167 GSC08973-01406 HD307300,ASASJ115305-6023.3 115305.073 -602317.46 10.00-10.31 10.00-10.31 OB-e(Stephenson&Sanduleak1971) U l SRO GCAS168 GSC08977-00310 HD103574,NSV19021 115521.663 -634212.81 7.90-8.01* 7.90-8.01 em(MacConnell1981),B2V(e)(Houk&Cowley1975) E l,s,u LTV BE169 GSC09234-02316 HD103715,NSV5395 115628.268 -713908.30 9.07-9.26* 9.07-9.26 em(Henize1976),B0/3:ne(Houk&Cowley1975),B2V?ne(Feastetal.1957) E l,u LTV,ObV GCAS170 GSC08973-01861 HD103872,GDS_J1157349-613259 115734.951 -613259.12 8.83-8.93* 8.83-8.93 em(Henize1976),B5eshell?(Houk&Cowley1975) M l,u LTV BE171 GSC08977-00421 HD309397,CPD-612828 115737.026 -615254.46 10.61-10.70 10.61-10.70 B9(Nesterovetal.1995),B7/8(Sundmanetal.1974) L LTV GCAS:172 GSC08978-01510 HD309467,GDS_J1202044-631522 120204.394 -631522.05 9.94-10.12* 9.94-10.12 Be(Stephenson&Sanduleak1977a) U l,u LTV BE173 GSC08974-01031 HD104552,NSV19130 120223.398 -612705.26 9.36-9.52* 9.36-9.53 em(Henize1976),B3/5e:(Houk&Cowley1975) M l,u ObV GCAS174 GSC08974-00327 CD-603989,GDS_J1207221-612424 120722.003 -612424.62 9.56-9.90* 9.56-9.90 OB(Münch1954),B6-7(Sundmanetal.1974) M ObV GCAS175 GSC08982-00852 CPD-632220 121637.856 -641720.08 10.35-10.56 10.35-10.56 em(Wray1966) U l LTV GCAS176 GSC08641-01826 HD106793,CPD-554964 121659.720 -562424.23 9.68-9.89* 9.66-9.89 B8/9IVe(Levenhagen&Leister2006),B7e(Stephenson&Sanduleak1977a) L l ObV GCAS177 GSC08974-00002 NSV19349,CPD-594156 121708.449 -604029.68 10.63-10.89* 10.63-10.89 B7e(Stephenson&Sanduleak1977a) L l ObV GCAS178 GSC08979-00623 CPD-622673 121809.428 -630113.42 9.37-9.48 9.33-9.48 B7e:(Stephenson&Sanduleak1977b) L l,u LTV GCAS179 GSC08975-03998 HD106960,CPD-603892 121813.632 -612930.86 9.50-9.61* 9.50-9.61 em(Henize1976),B8II/III(Houk&Cowley1975) L l ObV GCAS180 GSC08975-00799 HD107208,GDS_J1219489-603018 121948.955 -603018.34 8.94-9.10 8.94-9.10 B3II(Houk&Cowley1975),OB(Münch1954) E u LTV,EB EA+BE 1.68445(5)181 GSC08988-02966 HD109474,CPD-604167 123527.589 -611808.65 8.83-9.02* 8.83-9.02 em(Henize1976),B8Ib/II(Houk&Cowley1975) L l,s,u ObV GCAS182 GSC08992-01008 HD111124,CPD-622928 124750.751 -625945.28 9.27-9.42* 9.27-9.42 em(Henize1976),B1/3I:(Houk&Cowley1975) E l SRO,LTV GCAS183 GSC08988-01196 HD111363,CPD-604306 124927.495 -604156.82 8.80-9.11* 8.77-9.11 em(MacConnell1981),B3III(Houk&Cowley1975) E l,u ObV GCAS184 GSC08989-02518 HD312075,CPD-594513 125236.241 -601825.34 10.30-10.54* 10.30-10.70 em(Henize1976),B0(Cannon&Mayall1949) E l LTV GCAS185 GSC09001-00465 HD111906,CPD-661982 125341.623 -672415.84 9.42-9.56* 9.37-9.56 em(MacConnell1981),B3/5III/V(Houk&Cowley1975) M l LTV,NRP LERI 0.43626(3)186 GSC09245-01017 HD112442,CPD-691733 125806.815 -703249.24 9.26-9.42* 9.26-9.42 B5/6V(Houk&Cowley1975) M ObV GCAS187 GSC08660-01131 HD112825,ASASJ130024-5941.1 130023.895 -594107.60 9.53-9.78* 9.53-9.78 B1.5IVe(Jascheketal.1964),em(Henize1976) E l,u SRO GCAS188 GSC08660-00731 CPD-594679 130247.858 -595413.23 10.14-10.40* 10.14-10.42 Be(Johnstonetal.1992),pulsarcompanion,Be(Stephenson&Sanduleak1977a),B5(Stephenson&Sanduleak1977a),B8Ib(Kennedy1996),B2V:(Buscombe1998) U l ObV GCAS189 GSC08652-02075 HD113399,ASASJ130418-5610.6 130417.639 -561034.42 8.88-9.12 8.88-9.12 em(Henize1976),B7II(Houk&Cowley1975) L l ObV GCAS190 GSC08998-01018 HD114044,CPD-642199 130909.723 -645446.42 9.40-9.64* 9.40-9.64 B5V(Houk&Cowley1975) M ObV GCAS191 GSC09245-00106 HD114200,ASASJ131053-7048.5 131052.704 -704831.08 8.43-8.82* 8.43-8.82 B1IIIne(Garrisonetal.1977),B5Ve(Hilletal.1974),B0/2V:e(Houk&Cowley1975) E l,s ObV GCAS192 GSC08998-01663 HD114516,ASASJ131222-6348.7 131222.388 -634843.94 8.22-8.70* 8.22-8.70 em(Henize1976),B0V:e:(Houk&Cowley1975) E l SRO GCAS M N R A S , ( ) B e r nha r d e t a l . Table A1continued. (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)No. IDGSC IDalt α (J2000) δ (J2000) Range( V ) Range( V ) Spec.type subtype emission Var.type Var.type Period(s)[mag] lit.[mag] lit. [E/M/L/U] flag [LB17] [GCVS/VSX] [d]193 GSC08990-00217 HD115114,NSV19676 131616.119 -614544.17 9.69-9.92* 9.29-9.92 B1III:ne(Garrisonetal.1977),B0e(Humphreys1975) E l,u LTV GCAS194 GSC08995-02904 CPD-613736,ASASJ132922-6202.3 132922.315 -620217.42 9.49-9.95* 9.49-9.95 B2IVe(Garrisonetal.1977) E l ObV GCAS195 GSC07793-00222 CPD-385581 134445.709 -392900.84 9.82-10.11 9.82-10.15 OB1995PASP..107..846D,Be(Bidelman&MacConnell1973) U l LTV GCAS196 GSC09016-00519 HD119423 134518.398 -664516.78 7.35-7.60* 7.35-7.60 B3Vne(Levenhagen&Leister2006),B8e(Stephenson&Sanduleak1977a) M l,s,u ObV GCAS+LERI197 GSC09008-04083 HD119763,CPD-623579 134700.413 -630612.70 9.62-9.86* 9.55-9.86 em(MacConnell1981),B9IIKn(Houk&Cowley1975) L l LTV GCAS198 GSC08676-01771 HD120330,ASASJ135026-5944.8 135026.092 -594452.83 7.78-8.14* 7.72-8.14 B2/3Vnne(Houk&Cowley1975) E l,s ObV,LTV GCAS199 GSC09009-01997 HD122669,NSV20029 140522.036 -623026.63 8.94-9.02* 8.94-9.02 B1III:e(Garrisonetal.1977),B0.5IIep(Garrisonetal.1975),B0.5Ve(Crampton1971) E l,s,u LTV BE200 GSC09009-02487 HD122691,ASASJ140525-6235.4 140525.178 -623518.37 9.33-9.81 9.20-9.81 B1:Vnne(Garrisonetal.1977) E l SRO GCAS201 GSC09005-03448 CPD-614341,ASASJ140726-6143.2 140726.528 -614313.09 10.16-10.40* 10.16-10.42 OB-(Lynga1964) U ObV GCAS202 GSC09005-03474 Hen3-966,ASASJ140947-6145.0 140947.761 -614458.43 11.63-12.07 11.63-12.07 OBe(Stephenson&Sanduleak1977a) U l IP VAR 16.77(1)203 GSC09013-01063 CPD-633152,ASASJ141100-6427.6 141100.704 -642732.82 9.88-10.01* 9.88-10.01 Be:(Stephenson&Sanduleak1977b) U l ObV GCAS204 GSC09006-04576 CPD-605320,GDS_J1422173-603957 142217.323 -603957.20 9.64-9.84* 9.64-9.84 Be(Stephenson&Sanduleak1977a),Be(Bidelman&MacConnell1973) U l LTV,ObV GCAS205 GSC08691-03023 CPD-595640,ASASJ143516-5954.6 143516.240 -595437.65 10.56-10.80* 10.51-10.80 Be(Stephenson&Sanduleak1977a) U l SRO GCAS206 GSC08688-01283 HD129772,CPD-556162 144636.797 -562508.11 8.57-8.63* 8.55-8.63 em(MacConnell1981),B7/9IIIp:(Houk&Cowley1975),A2III:(Cannon&Pickering1920) L l,s LTV BE207 GSC09020-02147 CPD-595788,ASASJ150346-6021.9 150345.861 -602155.68 10.23-10.52* 10.23-10.52 OB-(Stephenson&Sanduleak1971) U SRO GCAS208 GSC07821-02254 NSV6905 150402.156 -382718.72 11.68-12.02* 11.68-12.03 U LTV,ObV GCAS209 GSC08305-02320 HD133901,CPD-507613 150852.450 -511025.57 9.21-9.36* 9.21-9.36 Beshell(Vennetal.1998),B8/9Iab(Houk1978),A5Ibe(Stephenson&Sanduleak1971) L l LTV BE210 GSC09436-00541 HD132875 151040.749 -802244.05 9.42-9.55* 9.40-9.55 B8II/III(e:)(Houk&Cowley1975) L l ObV GCAS211 GSC08702-00469 ALS19454,ASASJ151114-5724.8 151114.025 -572447.63 11.34-11.97 11.19-11.97 OB+e(Orsatti&Muzzio1980) U l ObV GCAS212 GSC09033-02403 HD134401,SAO253057 151312.155 -655809.02 8.89-8.98* 8.89-9.02 B2Vne(Levenhagen&Leister2006),B2IVnnep(shell)(Garrisonetal.1977),B2Vne(Houk&Cowley1975) E l,s,u LTV,NRP LERI+BE 0.423720(2)213 GSC08303-01041 HD136556,ASASJ152320-5007.0 152320.149 -500658.43 8.99-9.19 8.99-9.19 B2/3V:ne(Houk1978),B1Vne(Garrisonetal.1977),B:nne(Feastetal.1961) E l,s LTV,SRO: GCAS214 GSC07847-00082 HD136935,CPD-437060 152454.683 -440914.63 7.95-8.09 7.95-8.10 B6II(Houk1978),B8(SpencerJones&Jackson1939) U ObV GCAS215 GSC08307-01059 HD137837,CPD-508117 153023.229 -510939.72 9.00-9.19 9.00-9.19 B5/8II/III(Houk1978) M ObV GCAS216 GSC09022-00605 HD138131,ASASJ153311-6054.6 153311.287 -605433.69 8.99-9.19* 8.99-9.19 B6Vne(Houk&Cowley1975) M l ObV GCAS217 GSC08701-00997 HD142237,NSV20435 155605.974 -545709.55 8.75-8.94 8.63-8.94 B1Vne(Levenhagen&Leister2006),Be(Stephenson&Sanduleak1977a),B2Vne(Houk&Cowley1975),B3Ve(Humphreys1975) E l,u,s ObV GCAS218 GSC08719-02158 HD146261,CPD-577793 161824.885 -574932.97 9.13-9.32* 9.13-9.32 B8/9II(Houk&Cowley1975),B5V(Feast1957) L ObV GCAS219 GSC08319-00698 HD146444,NSV20575 161839.380 -492449.94 7.47-7.75* 7.47-7.75 B2Ve(A&),B2Vne(Houk1978) E l,s ObV,LTV GCAS220 GSC08719-00464 HD146324,CPD-577816 161849.010 -575551.54 7.68-7.99* 7.68-7.99 em(Henize1976),B5V(e)(Feast1957) M l,u,s LTV GCAS221 GSC08711-02092 HD146596,GDS_J1619426-524618 161942.669 -524619.00 8.03-8.11 7.98-8.11 B5IV/V(e)(Houk1978),em(Henize1976) M l,s LTV BE222 GSC08723-00042 HD146531,CPD-577866 161955.512 -581001.86 9.72-9.78* 9.69-9.80 B3Ve(Levenhagen&Leister2006),B5/7III(Houk&Cowley1975) M l,u LTV BE223 GSC08715-01941 HD147302,CPD-557498 162401.276 -552713.35 7.65-7.74* 7.65-7.74 B2Vn(Garrisonetal.1977),B2III:n(e?)(Houk&Cowley1975) E l,s NRP LERI 0.510717(3)224 GSC08712-02498 CPD-537997,ASASJ162749-5332.1 162748.809 -533205.05 9.59-9.89* 9.59-9.89 B2.5IVn(e)(Garrisonetal.1977) E l,u SRO GCAS225 GSC08325-05810 HD148567,ASASJ163103-4628.8 163102.812 -462845.72 7.84-8.02* 7.84-8.11 B2II:neshell?(Houk1978),B1IIIne(Garrisonetal.1977) E l,s ObV,NRP GCAS+LERI 0.789476(9)226 GSC09042-01527 HD148907,CPD-615734 163514.063 -615340.15 9.26-9.36* 9.26-9.36 B7e(Stephenson&Sanduleak1977a),B5/7V(Houk&Cowley1975) M l ObV GCAS227 GSC08337-00341 HD149814,CPD-519804 163950.025 -520715.89 9.09-9.16* 9.05-9.16 B5/7III/V(Houk1978),em(Henize1976) M l,s LTV BE228 GSC08325-00916 HD328684,ASASJ164052-4639.0 164052.280 -463902.31 10.37-10.73* 10.37-10.73 em(Vegaetal.1980),A2(Nesterovetal.1995) U l ObV GCAS229 GSC08330-05153 HD150231,CD-4710953 164152.647 -472249.32 9.02-9.41* 9.02-9.41 em(MacConnell1981),B3V(Houk1978) E l ObV,NRP GCAS+LERI 0.580790(7)230 GSC08338-02080 HD151083,ASASJ164751-5146.1 164751.392 -514603.99 8.78-9.36* 8.78-9.36 B2Vn(e)(Houk1978),B1:IIInne(Garrisonetal.1977) E l,u,s ObV GCAS231 GSC08734-02077 HD151873,CPD-567887 165321.134 -570135.38 9.08-9.21 9.08-9.21 em(Henize1976),A(e)pshell(Houk&Cowley1975),Bshell(Bidelman&MacConnell1973) L l ObV GCAS232 GSC07872-00681 HD322282,NSV20824 165429.032 -404117.37 8.90-9.06* 8.87-9.06 em(Henize1976),OBe(Stephenson&Sanduleak1971),Be(Merrill&Burwell1949) U l,u,s ObV GCAS233 GSC07872-00390 HD322447,NSV20862 165618.014 -404048.78 8.77-8.90* 8.77-8.92 em(Henize1976),B1IV(Schildetal.1969) E l ObV BE234 GSC08328-00373 HD155280,CPD-468449 171250.342 -462619.44 8.48-8.76* 8.48-8.76 B2/3II(Houk1978);B3III(Garrisonetal.1977) E u,s SRO GCAS235 GSC07878-00246 HD155352,ASASJ171300-4238.0 171300.391 -423800.42 8.17-8.47* 8.17-8.47 B2V(Houk1978);Be(Bidelman&MacConnell1973) E l,u,s ObV GCAS236 GSC08345-03046 HD156008,CPD-478152 171730.679 -474422.49 9.53-9.63* 9.52-9.63 B8IV(Houk1978),em(Henize1976) L l LTV BE237 GSC07374-00838 NSV21486,CPD-356938 172026.473 -354406.88 10.09-10.27 10.09-10.70 em(Henize1976),OBe(Stephenson&Sanduleak1971),B0.5:Ve(Roslund1966) E l ObV BE238 GSC07366-00860 CPD-324502,ASASJ172148-3304.8 172147.648 -330448.74 10.66-11.03 10.66-11.03 em(Henize1976),OB-(Stephenson&Sanduleak1971) U l SRO GCAS239 GSC08341-00889 HD157115,ASASJ172336-4526.3 172336.284 -452618.90 8.42-8.62* 8.42-8.62 B5IV(Houk1978) M ObV GCAS240 GSC07375-00048 HD157829,CPD-294703 172655.205 -300530.87 8.68-8.88* 8.68-8.88 B3III/IV(Houk1982),em(A&) E l ObV,LTV GCAS241 GSC08342-00052 HD157847,CPD-458603 172800.368 -454515.65 9.41-9.58* 9.41-9.58 B9Ib(Houk1978),em(MacConnell1981) L l ObV GCAS242 GSC07384-00247 HD320103,ASASJ173632-3403.8 173631.591 -340347.71 10.40-10.67 10.40-10.69 em(Henize1976),OBe(Stephenson&Sanduleak1971) U l ObV GCAS243 GSC08342-01635 HD159489 173713.837 -450926.63 7.98-8.26* 7.98-8.26 B1Ve(Levenhagen&Leister2006),B3V(e)p(shell)(Garrisonetal.1977) E l,u ObV GCAS244 GSC06835-00151 CPD-285745,ASASJ173920-2805.7 173919.633 -280539.42 11.08-11.30 11.08-11.30 OB-e(Stephenson&Sanduleak1971) U l ObV GCAS245 GSC06839-00611 CD-2913831,ASASJ173930-2947.7 173929.975 -294742.08 10.59-11.07* 10.59-11.07 OB+e(Stephenson&Sanduleak1971) U l SRO GCAS246 GSC07889-01252 HD160751,CPD-397553 174331.964 -394920.33 8.59-8.71* 8.50-8.71 B7/8II(Houk1982) L LTV,ObV GCAS247 GSC07385-01338 HD161774,CPD-334618 174851.346 -335145.05 8.64-8.76 8.64-8.72 B8Vnne(Levenhagen&Leister2006),B5:V:nne(Houk1982) L l,u,s LTV,NRP LERI 0.410651(4)248 GSC07886-02848 HD162352 175218.591 -374501.99 8.21.8.30* 8.21-8.31 B2/3ne:(Houk1982),B1.5Vn(e)(Garrisonetal.1977) E l,s LTV,NRP LERI 0.612158(6)249 GSC06853-01718 ASASJ175438-2926.8 175438.171 -292646.64 11.57-12.42* 11.57-12.42 OB-e:(Stephenson&Sanduleak1977b) U l ObV GCAS250 GSC06853-02519 HD163453,NSV24052 175725.827 -281518.41 9.23-10.10* 9.23-10.10 Bnne(Houk1982),em(Henize1976) U l ObV GCAS251 GSC06841-01725 ALS4506,ASAS175746-2412.2 175746.409 -241209.47 11.11-11.33* 11.11-11.33 em(Kohoutek&Wehmeyer2003),OB(Stephenson&Sanduleak1971) U l ObV GCAS252 GSC06846-01106 HD314947,ASASJ180235-2541.7 180234.984 -254143.53 10.26-10.44 10.17-10.44 em(Henize1976),Be(Velghe1957) U l LTV,ObV GCAS253 GSC07399-01124 HD165248,CPD-347582 180631.633 -343052.00 9.30-9.38* 9.30-9.38 B3/5V:(Houk1982) M LTV BE254 GSC06263-03157 HD165595,CPD-226704 180738.231 -220657.46 8.45-8.50 8.45-8.50 B3(Cannon&Mayall1949) E u LTV,NRP LERI 0.540456(6)255 GSC07399-01226 HD321289,ASASJ180801-3524.2 180800.469 -352415.29 9.90-10.24* 9.90-10.24 B5e(Stephenson&Sanduleak1977a) M l SRO GCAS256 GSC06272-02199 HD165970,CPD-196497 180915.914 -194323.86 8.96-9.16* 8.96-9.16 B5e(Stephenson&Sanduleak1977a) M l ObV GCAS M N R A S , ( ) n i n ve s ti ga ti ono ft h e pho t o m e t r i cv a r i ab ilit y o f c onfi r m e dand c and i da t e G a l a c ti c B e s t a rs u s i ng A S A S - t a Table A1continued. (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)No. IDGSC IDalt α (J2000) δ (J2000) Range( V ) Range( V ) Spec.type subtype emission Var.type Var.type Period(s)[mag] lit.[mag] lit. [E/M/L/U] flag [LB17] [GCVS/VSX] [d]257 GSC06268-02490 HD166188,ASASJ181018-1811.7 181018.319 -181141.36 8.78-9.06* 8.78-9.06 B2V:ep(Morganetal.1955) E l,s SRO GCAS258 GSC06276-00317 HD166146 181018.747 -222314.69 9.88-9.98* 9.88-9.98 B8(Cannon&Mayall1949) L LTV GCAS259 GSC06851-02063 HD166365 181127.175 -270802.62 10.14-10.26* 10.14-10.26 B9II/III(Houk1982),B7e:(Stephenson&Sanduleak1977b) L l ObV GCAS260 GSC06847-02930 HD315277,ASASJ181208-2508.5 181208.042 -250832.83 10.85-11.15 10.85-11.15 OB+e(Stephenson&Sanduleak1971),Be(Miller&Merrill1951) U l ObV,LTV GCAS261 GSC06851-04189 HD166629 181238.466 -270829.26 9.10-9.37* 9.10-9.37 B5nne(Houk1982),B9e(Merrill&Burwell1949) U l ObV GCAS262 GSC06268-00943 HD312861,ASASJ181307-1821.5 181307.086 -182131.63 10.03-10.19* 10.03-10.20 B7e(Stephenson&Sanduleak1977a) L l ObV GCAS263 GSC06847-02073 HD166967,CPD-256403 181408.185 -251839.00 8.36-8.48* 8.35-8.48 OB(Stephenson&Sanduleak1971),B5e(Merrill&Burwell1949) M l,u,s LTV GCAS264 GSC06272-00394 HD167247,ASASJ181501-1912.5 181501.126 -191227.66 9.10-9.20* 9.10-9.20 B5III/V(Houk1978),B9(Yale1997) U LTV GCAS265 GSC07404-05201 HD167233,NSV24347 181550.905 -363425.55 6.57-7.02* 6.57-7.02 B3Ve(A&),B3Ve(Buscombe&Kennedy1969) E l,s ObV GCAS266 GSC06269-02592 ALS4888,ASASJ181806-1728.9 181805.938 -172854.73 10.59-11.00 10.59-11.00 OB(Stephenson&Sanduleak1971),em(Henize1976) U l ObV GCAS267 GSC06274-00902 HD313306,ASASJ182441-1940.4 182441.455 -194025.02 9.61-9.84* 9.59-9.84 A0(Cannon&Mayall1949) L ObV GCAS268 GSC07909-02656 HD169639 182733.814 -413533.39 10.29-10.46 10.23-10.46 em(MacConnell1982),B8/9Ib/II(Houk1978) L l LTV GCAS269 GSC05703-02553 HD170603,BD-154995 183054.729 -145539.85 9.24-9.54* 9.24-9.54 B3V(Hiltner&Iriarte1955) E ObV GCAS270 GSC05124-01543 ASASJ183442-0638.8 183442.525 -063849.26 11.68-11.87 11.68-11.87 B5(Roslund1963) M LTV GCAS271 GSC05703-01526 HD171392,ASASJ183506-1419.8 183505.696 -141950.09 9.09-9.38 9.09-9.38 OB(Nassau&Stephenson1963) U SRO,LTV GCAS272 GSC06275-00943 HD172122,ASASJ183912-2020.1 183912.148 -202008.58 8.62-8.87 8.62-8.87 B(Stephenson&Sanduleak1977a),B2IVnpshell(Garrisonetal.1977) E l,s LTV GCAS273 GSC05692-01642 HD172637,ASASJ184139-0803.3 184138.802 -080315.26 9.27-9.38* 9.27-9.38 OB(Nassau&Stephenson1963),B3(Roslund1963) E ObV GCAS274 GSC05125-02006 ALS9887,ASASJ184244-0609.2 184244.504 -060913.63 10.32-10.66* 10.32-10.66 em(MacConnell1981),B3(Roslund1963) E l ObV GCAS275 GSC00456-00461 HD173530 184542.914 +043442.98 8.79-8.89* 8.79-8.89 B8II/IIIe(Stephenson&Sanduleak1977a) L l LTV BE276 GSC05693-07523 TYC5693-7523-1 184631.795 -073836.51 11.77-12.05* 11.77-12.05 U ObV GCAS277 GSC05126-03377 ASASJ184740-0630.6 184739.672 -063039.80 11.04-11.47* 11.04-11.47 em:(Stephenson&Sanduleak1977b) U l SRO GCAS278 GSC05701-00964 HD174070,SAO161859 184912.383 -123543.96 9.09-9.22* 9.09-9.22 em(MacConnell1981),B4(Neubauer1943) M l,u ObV GCAS279 GSC01026-02065 HD174571,ASASJ185047+0842.2 185047.173 +084210.05 8.67-8.86 8.67-8.92 Beshell?(Stephenson&Sanduleak1977a),B2.5V:[n]e(Walborn1971),B2e(Vieiraetal.2003) E l,u ObV GCAS280 GSC06289-02980 HD174652,CPD-207256 185216.482 -201852.91 9.03-9.20 9.02-9.20 B9e(Merrill&Burwell1949) L l ObV GCAS281 GSC05123-00145 HD175180,ASASJ185427-0522.8 185426.577 -052248.43 8.92-9.18 8.92-9.18 B3III(Houk&Swift1999) E ObV GCAS282 GSC00463-02825 HD178720 190937.901 +005529.49 8.88-9.11* 8.88-9.11 B2e(Bidelman1981) E l,u,s ObV GCAS283 GSC05131-01423 SAO143395 192615.407 -001516.29 9.19-9.29* 9.19-9.29 B2(Kelly&Kilkenny1986) E ObV GCAS284 GSC02129-00864 HD338423,ASASJ192626+2431.4 192626.254 +243121.95 11.38-11.60 11.38-11.60 em(Coyneetal.1974),A2(Cannon&Mayall1949) L l ObV: BE:285 GSC05149-01177 HD185092,NSV24828 193736.523 -024156.43 8.56-8.72 8.56-8.72 B8Ib(Anderson&Francis2012) L ObV GCAS286 GSC01645-00281 HD347184 203830.165 +211943.96 9.08-9.38 9.10-9.38 em(MacConnell1982) U l ObV GCAS287 GSC01124-01184 BD+084699 213523.790 +092918.45 10.07-10.37* 10.07-10.37 B8(Wrightetal.2003) L LTV GCAS M N R A S , ( ) Bernhard et al.
APPENDIX B: LIGHT CURVES
MNRAS000
MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure B1.
The ASAS-3 light curves of all sample stars ( N = 287). For convenience and to provide an easy identification in the corresponding tables (TablesA1 and D1), all stars were numbered in order of increasing right ascension (No. 1 – No. 287).MNRAS , 1–46 (2017) Bernhard et al.
Figure B1. continued. MNRAS000
Figure B1. continued. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure B1. continued.MNRAS , 1–46 (2017) Bernhard et al.
Figure B1. continued. MNRAS000
Figure B1. continued. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure B1. continued.MNRAS , 1–46 (2017) Bernhard et al.
Figure B1. continued. MNRAS000
Figure B1. continued. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure B1. continued.MNRAS , 1–46 (2017) Bernhard et al.
Figure B1. continued. MNRAS000
Figure B1. continued. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure B1. continued.MNRAS , 1–46 (2017) Bernhard et al.
Figure B1. continued. MNRAS000
Figure B1. continued. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure B1. continued.MNRAS , 1–46 (2017) Bernhard et al.
Figure B1. continued. MNRAS000
Figure B1. continued. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure B1. continued.MNRAS , 1–46 (2017) Bernhard et al.
Figure B1. continued. MNRAS000
Figure B1. continued. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure B1. continued.MNRAS , 1–46 (2017) Bernhard et al.
Figure B1. continued. MNRAS000
Figure B1. continued. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure B2.
Phase plots of the stars showing periodic variability. For the construction of the plots, ASAS-3 data have been folded with the periods listed in TableA1. In order to bring out the periodic variability more clearly in objects that show complex photometric variations, some plots have been based on only part ofthe ASAS-3 observations, as indicated below the abscissae. All other plots have been based on the full available range of data. To facilitate identification, theinternal running numbers are provided in the plots (upper left).MNRAS , 1–46 (2017) Bernhard et al.
Figure B2. continued. MNRAS000
Figure B2. continued. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data APPENDIX C: NEWLY-ACQUIRED AND ARCHIVALSPECTRA
MNRAS , 1–46 (2017) Bernhard et al.
Figure C1.
The classification resolution spectra obtained at Mirranook Observatory and the available LAMOST spectra of our sample stars, illustrating theregion containing the H α and H β lines (4700–7100 Å). In order to save space, unit labeling has been omitted from the abscissae and ordinates, which denote,respectively, wavelength (Å) and normalized flux in arbitrary units. Objects have been sorted by increasing right ascension. To facilitate identification, theinternal running numbers are provided in the plots. MNRAS000
The classification resolution spectra obtained at Mirranook Observatory and the available LAMOST spectra of our sample stars, illustrating theregion containing the H α and H β lines (4700–7100 Å). In order to save space, unit labeling has been omitted from the abscissae and ordinates, which denote,respectively, wavelength (Å) and normalized flux in arbitrary units. Objects have been sorted by increasing right ascension. To facilitate identification, theinternal running numbers are provided in the plots. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Figure C1. continued.MNRAS , 1–46 (2017) Bernhard et al.
Figure C1. continued. MNRAS000
Figure C1. continued. MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data E ( b - y ) , m a g E(B-V), mag E ( B - V ) ( U B V ) , m a g E(B-V) (spectroscopic), mag -0.35 -0.30 -0.25 -0.20 -0.15 -0.10-0.15-0.10-0.05 ( b - y ) (B-V) Figure D1.
The top panel compares the uvby -based and
UBV -based inter-stellar colour excesses, as obtained following Crawford (1978) and Crawford(1994), respectively. We derive E ( b − y ) = . ± . E ( B − V ), whichagrees well with the established coefficient of 0.74 between the two colourexcesses. The middle panel illustrates the comparison between the colour ex-cesses derived from UBV photometry and spectral classification; the agree-ment is satisfactory. The bottom panel provides a comparison of the dered-dened indices ( B − V ) and ( b − y ) . The correlation between these twoquantities is very good (standard error ± . mag). The solid lines in theupper and bottom panels represent the best fits to the data; the solid line inthe middle panel is the unity line. APPENDIX D: INTRINSIC COLOURS ANDINTERSTELLAR COLOUR EXCESSES FROM
UBV
AND
UVBY
PHOTOMETRIES
As Be stars enter a mass-losing phase, their colours are prone tochange continuously. de Wit et al. (2006) have found that the out-flowing material produces a bi-valued colour-magnitude relation inmany Small Magellanic Cloud Be stars that leads to loop structuresin colour-magnitude diagrams and can be ascribed to optical deptheffects. Likewise, complex colour changes have been observed inGalactic Be stars, which – depending on the inclination angle – maybecome redder or bluer as their brightness increases (e.g. Hirata1982; Percy & Bakos 2001; Keller et al. 2002). Marr et al. (2018)have investigated variations in linear polarization and V and B bandcolour-magnitudes for classical Be star disks and found that, de-pending on the employed model, the maximum changes in ( B − V )do not exceed 0.1 mag. Be stars, therefore, are not particularly well suited to determineparameters like interstellar colour excess. On the other hand, inter-stellar colour excesses obtained via uvby photometry for classicalBe stars have been shown to be consistent with colour excessesbased on the Barbier-Chalonge-Divan spectrophotometric system(Gkouvelis et al. 2016), and, given the large sample size and theavailability of good-quality optical photometry for a significant partof our sample, we have chosen to investigate the possibilities ofcolour excess determination with our sample stars.Of all 287 objects, 64 stars boast uvby photometry and 149 starshave complete
UBV data in either the GCPD (Mermilliod et al.1997) and/or Paunzen (2015). The
UBV -based colour excess E ( B − V ) was obtained following the procedure summarized byCrawford (1994) and also the more recent calibrations derived byPecaut & Mamajek (2013). Both calibrations provide similar re-sults. The uvby -based colour excess E ( b − y ) was obtained via thecalibrations of Crawford (1978). Spectral types are available for 72%of our sample stars. Using this information, we also obtained intrin-sic ( B − V ) colours utilizing the calibration of Deutschman et al.(1976). Since uncertainties and variations in spectral type and lumi-nosity class are a general characteristic of Be stars (cf. Section 2.3),we made efforts to adopt the most reliable classification for each starby evaluating the quality of the classification’s source. In general,the most recent classification was adopted, and classifications fromspectroscopic surveys were favoured.Figure D1 provides comparisons between the colour excessesas derived by the different methods applied here. The top panelshows a comparison between the uvby -based and UBV -based colourexcesses, the latter obtained following Crawford (1994). From this,we derive E ( b − y ) = . ± . E ( B − V ), which agrees well withthe established coefficient of 0.74 between the two colour excesses(cf. e.g. Straižys 1992). This implies a good agreement betweenthese two sets of photometry-based colour excesses, suggesting thatthe (constant) colour excess due to interstellar absorption is consid-erably larger than the mean colour changes induced by the variabilityof our sample stars. This is in line with results from the literature(e.g. de Wit et al. 2006). We also note that, even in the most variablestars of our sample, the mean V magnitude difference between twoobservations at any randomly-chosen epochs during the whole timespan of observations amounts to only about 0.1 mag. We thereforeexpect corresponding changes in ( B − V ) on the order of 0.025 mag,which is on the upper limit of the calculations of Marr et al. (2018).This is in agreement with the here reported scatter for the intrinsiccolours.The calibration by Pecaut & Mamajek (2013) also provides agood agreement with the uvby colour excesses, but a slightly smallervalue of the established coefficient. Because of this we give prefer-ence to the E ( B − V ) values based on Crawford (1994). The middlepanel shows a comparison between the colour excesses derived from UBV photometry and spectral classification; the agreement is sat-isfactory. The majority of our sample stars have interstellar colourexcesses E ( B − V ) between 0.2 and 0.6 magnitudes.Figure D1 bottom panel provides a comparison of the dered-dened indices ( B − V ) and ( b − y ) . Despite the scatter inducedby the changing colours of Be stars, the correlation between thesetwo quantities is strong (standard error ± . mag), which makesus confident of the applicability of our approach. We thereforecalculated a combined ( B − V ) index based on an average of In this section, the term colour excess always refers to interstellar colourexcess.MNRAS , 1–46 (2017) Bernhard et al.
Figure D2.
A comparison between the combined ( B − V ) index as calculatedin the present work and the intrinsic ( B − V ) colours derived from the spectraltypes. The solid line represents the best fit to the data; the dashed line is theunity line. both indices, where available. To this end, we used the relation( B − V ) = ( b − y ) /0.436 to convert the ( b − y ) values to ( B − V ) ,which was obtained based on our comparisons. A comparison be-tween this index and intrinsic ( B − V ) colours derived from thespectral types is provided in Fig. D2. The resulting correlation ismediocre, which we attribute mostly to the lower precision of thespectrophotometric intrinsic colour determinations and the knowninaccuracies in the spectral classification of Be stars (cf. Section2.3). Table D1 lists the derived colour indices and colour excessesfor our sample stars. We note that for three objects in our sample,the ( B − V ) index from Kharchenko (2001) deviates from the ( B − V )index taken from the GCPD and/or APASS by more than 0.5 mag.These objects are GSC 08702-00469 ( ∼ ∼ ∼ V ∼ ∼ B − V ) indices, but only general spectral types such as Be, OBe orem. The results are shown in Fig. D3 and are fully consistent withthe results based on spectral type. Stars bluer than ( B − V ) ≈ − . show more frequent outbursts. This corresponds to a spectral typeof ∼ B4 (Ducati et al. 2001), which defines the red border of the hereemployed definition of early-type Be stars (Be stars with spectraltypes earlier than B4; cf. Section 2.3). In fact, some of the most outlying points in Fig. D2 relate to objectiveprism spectra taken more than 60 years ago.
Figure D3.
Outbursts per year versus average ( B − V ) index, as derived fromthe available UBV and uvby data. The 24 stars that boast good photometry,and thus ( B − V ) indices, but only general spectral types such as Be, OBeor em (and hence are not considered in Fig. 14) are indicated by crosses.This paper has been typeset from a TEX/L A TEX file prepared by the author.MNRAS000
Outbursts per year versus average ( B − V ) index, as derived fromthe available UBV and uvby data. The 24 stars that boast good photometry,and thus ( B − V ) indices, but only general spectral types such as Be, OBeor em (and hence are not considered in Fig. 14) are indicated by crosses.This paper has been typeset from a TEX/L A TEX file prepared by the author.MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Table D1.
Colour indices and colour excesses for our sample stars, sorted by increasing right ascension. The columns denote: (1) Internal identification number.Stars were numbered in order of increasing right ascension. (2) Identification from the Guide Star Catalog (GSC), version 1.2. (3) ( B − V ) index, taken fromKharchenko (2001). (4) ( B − V ) index, taken from the GCPD and/or APASS. When indices from both sources are available, average values have been given. (5)( U − B ) index, taken (with very few exceptions) from the GCPD. (6) Spectral type and luminosity class used as input for obtaining the spectroscopic ( B − V ) and E ( B − V ). (7) ( B − V ) index, as derived from the spectral type. (8) Average ( B − V ) index, as derived from the available UBV and uvby data. (9) Colourexcess E ( B − V ), as derived from spectroscopy. (10) Average colour excess E ( B − V ), as derived from the available UBV and uvby data.(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)No GSC ( B − V ) ( B − V ) ( U − B ) SpT&LC ( B − V ) ( B − V ) E ( B − V ) E ( B − V )Kh01 GCPD GCPD input spec. phot. avg. spec. phot. avg.APASS1 GSC 06464-00405 -0.10 -0.15 -0.53 B3V -0.22 -0.14 0.12 -0.012 GSC 01845-02192 0.17 0.20 -0.51 B3IV -0.22 -0.22 0.39 0.423 GSC 08877-00138 -0.17 -0.18 -0.71 B5V -0.18 -0.21 0.01 0.034 GSC 04755-00818 0.11 0.03 – B9V -0.08 – 0.19 –5 GSC 09162-00751 0.20 0.09 -0.67 B2.5V -0.24 -0.25 0.43 0.346 GSC 00115-01423 -0.08 -0.10 -0.53 B6V -0.16 -0.16 0.08 0.067 GSC 01310-01587 0.08 – – – – – – –8 GSC 01311-01238 0.17 0.14 -0.69 B1V -0.28 -0.27 0.45 0.419 GSC 06491-00717 -0.09 – – B8V -0.12 – 0.02 –10 GSC 01868-01264 -0.02 0.16 – – – – – –11 GSC 00721-02056 0.15 – – B2V -0.26 – 0.40 –12 GSC 01864-00314 0.26 0.52 -0.45 – – -0.28 – 0.8013 GSC 00738-01213 0.57 0.65 – – – – – –14 GSC 00742-01475 0.82 0.75 – – – – – –15 GSC 00739-01143 0.27 0.30 – – – – – –16 GSC 00739-01342 0.13 – – B8V -0.12 – 0.25 –17 GSC 01319-00734 0.37 0.55 -0.57 – – -0.32 – 0.8718 GSC 00743-02467 0.04 0.09 -0.49 B8V -0.12 -0.19 0.15 0.2819 GSC 00732-02105 0.14 0.13 -0.75 B1V -0.28 -0.28 0.42 0.4120 GSC 00154-02436 0.28 0.30 -0.50 B0V -0.32 -0.24 0.59 0.5421 GSC 00733-01509 0.06 0.13 -0.69 B1V -0.28 -0.27 0.34 0.3822 GSC 00733-01932 0.24 0.43 – B3V -0.22 – 0.46 –23 GSC 00146-01543 0.17 0.27 – B5V -0.18 -0.18 0.35 0.3524 GSC 00154-00165 0.12 0.10 – B8V -0.12 – 0.24 –25 GSC 00755-00857 -0.06 0.14 – – – – – –26 GSC 00152-00780 0.35 0.35 – – – – – –27 GSC 00148-02601 0.17 0.20 -0.18 – – -0.11 – 0.3128 GSC 00160-01058 0.03 0.23 -0.72 B2V -0.26 -0.30 0.29 0.5329 GSC 05387-01121 -0.12 -0.13 -0.78 B5V -0.18 -0.22 0.06 0.0830 GSC 04801-00017 0.41 0.61 – – – – – –31 GSC 05383-00187 0.00 – – B8V -0.12 -0.13 0.12 0.0732 GSC 04805-00043 0.24 0.24 -0.70 B0.5V -0.30 -0.29 0.53 0.5333 GSC 05388-01118 0.52 0.51 – – – – – –34 GSC 00748-01908 -0.05 0.01 – – – – – –35 GSC 04809-00545 0.27 0.18 -0.75 B3V -0.22 -0.30 0.49 0.4836 GSC 00153-00891 -0.30 0.51 – – – – – –37 GSC 04801-01915 0.02 0.15 – B5V -0.18 – 0.20 –38 GSC 04826-00257 0.08 0.22 – – – – – –39 GSC 04826-01079 0.18 0.25 – – – – – –40 GSC 05393-02168 0.80 0.98 -0.05 – – -0.27 – 1.2641 GSC 05968-03899 0.01 0.02 – B7/8V -0.13 – 0.14 –42 GSC 05398-01016 0.07 0.09 -0.57 B2V -0.26 -0.22 0.33 0.2943 GSC 05973-00249 0.10 0.22 -0.74 B2V -0.26 -0.30 0.36 0.5244 GSC 05399-00962 0.01 0.01 -0.33 B8V -0.12 -0.11 0.12 0.1245 GSC 07634-01561 0.12 – – B8V -0.12 – 0.24 –46 GSC 04820-02947 -0.09 0.00 – B7V -0.14 – 0.05 –47 GSC 05978-01855 0.01 0.04 -0.50 B2.5V -0.24 -0.18 0.24 0.2248 GSC 05978-00030 0.63 – – – – – –49 GSC 05983-00995 0.08 0.16 – B5V -0.18 – 0.26 –50 GSC 07109-00828 0.18 0.20 -0.72 – – -0.29 – 0.4951 GSC 05405-00431 -0.02 – – B3V -0.22 -0.25 0.20 0.1952 GSC 05988-00265 0.32 0.41 -0.62 – – -0.31 – 0.7253 GSC 08552-00688 -0.07 -0.05 -0.81 B2V -0.26 -0.26 0.19 0.2154 GSC 06552-00580 0.52 – – – – – –55 GSC 06552-01189 0.31 0.36 -0.66 – – -0.31 – 0.6756 GSC 07106-02534 0.35 0.53 -0.42 – – -0.27 – 0.80MNRAS , 1–46 (2017) Bernhard et al.
Table D1. continued.(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)No GSC ( B − V ) ( B − V ) ( U − B ) SpT&LC ( B − V ) ( B − V ) E ( B − V ) E ( B − V )Kh01 GCPD GCPD input spec. phot. avg. spec. phot. avg.APASS57 GSC 07123-00519 0.57 1.03 -0.15 – – -0.30 – 1.3358 GSC 08135-03248 -0.01 – – B2V -0.26 -0.22 0.24 0.2259 GSC 06565-01179 0.42 0.45 -0.67 B0V -0.32 -0.33 0.73 0.7860 GSC 07124-01160 1.00 -0.29 – – -0.34 – 1.3461 GSC 07120-02077 0.40 0.44 -0.73 B1V -0.28 -0.35 0.68 0.7962 GSC 06562-00688 0.03 0.11 – A3V 0.08 – -0.05 –63 GSC 05421-00568 0.06 -0.05 – – – – – –64 GSC 07659-01614 0.32 – – – – – –65 GSC 05438-00850 -0.09 -0.11 -0.39 B3V -0.22 -0.10 0.14 0.0166 GSC 07125-02097 0.21 0.45 -0.66 B0V -0.32 -0.33 0.53 0.7867 GSC 05435-00526 -0.13 -0.15 – B7IV -0.14 – 0.01 –68 GSC 07669-01154 0.73 – – – – – –69 GSC 07669-03714 -0.17 -0.07 -0.97 B2V -0.26 -0.31 0.08 0.2470 GSC 07139-02209 0.31 – – A0IV -0.02 – 0.33 –71 GSC 08151-01868 0.20 0.23 -0.60 B2V -0.26 -0.26 0.46 0.4972 GSC 08155-02404 0.17 0.27 -0.74 B1.5V -0.27 -0.31 0.43 0.5873 GSC 08164-01530 0.08 – – B1V -0.28 – 0.36 –74 GSC 08594-00620 -0.02 -0.05 -0.68 B3V -0.22 -0.22 0.20 0.1875 GSC 08165-00324 0.26 0.32 -0.49 B2V -0.26 -0.24 0.51 0.5676 GSC 08582-02609 0.71 – – – – – – –77 GSC 08591-00039 0.02 -0.07 -0.84 B1IV -0.28 -0.27 0.30 0.2078 GSC 07686-01898 0.15 0.19 – B7V -0.14 – 0.29 –79 GSC 08587-02162 0.09 0.13 -0.75 B2IV -0.26 -0.29 0.35 0.4080 GSC 08174-00235 0.26 0.29 -0.41 B5V -0.18 -0.21 0.44 0.5081 GSC 09196-00424 0.89 – – – – – –82 GSC 08588-02569 0.16 0.20 -0.57 B4V -0.20 -0.24 0.36 0.4483 GSC 08167-01520 0.20 0.25 -0.75 – – -0.32 – 0.5784 GSC 08593-01904 0.07 0.09 -0.66 B2V -0.26 -0.24 0.33 0.3385 GSC 08585-02212 0.11 0.08 -0.76 B1.5V -0.27 -0.28 0.38 0.3586 GSC 08593-00336 0.01 -0.01 – B8/9V -0.10 – 0.11 –87 GSC 07179-02573 0.00 – – B8V -0.12 – 0.11 –88 GSC 08593-02269 -0.05 -0.01 -0.73 B2.5V -0.24 -0.25 0.19 0.2589 GSC 08606-00053 0.06 – B4V -0.20 – 0.26 –90 GSC 08598-02245 0.11 0.19 -0.58 B3IV -0.22 -0.24 0.33 0.4391 GSC 08606-02020 0.64 0.66 -0.41 – – -0.30 – 0.9692 GSC 08610-03102 -0.05 – – B5V -0.18 – 0.14 –93 GSC 08603-00164 0.33 0.25 -0.63 – – -0.27 – 0.5294 GSC 08599-02357 0.07 0.12 -0.64 B5V -0.18 -0.24 0.25 0.3695 GSC 08611-01377 -0.09 -0.09 – B2V -0.26 -0.21 0.17 0.0996 GSC 08603-00677 0.59 0.61 – B7V -0.14 – 0.73 –97 GSC 08955-00160 0.04 – – B4V -0.20 – 0.24 –98 GSC 08943-00584 -0.02 0.02 – B5V -0.18 – 0.16 –99 GSC 08607-01004 1.51 – – – – – –100 GSC 08607-00285 0.43 0.52 -0.58 B1V -0.28 -0.32 0.71 0.84101 GSC 08604-00356 0.15 – – B6.5V -0.15 – 0.30 –102 GSC 08947-00809 0.14 0.09 -0.90 – – -0.32 – 0.41103 GSC 08943-02244 -0.05 0.08 -0.93 B0V -0.32 -0.33 0.26 0.41104 GSC 08943-00620 0.16 0.32 -0.75 B2V -0.26 -0.33 0.41 0.65105 GSC 08612-00975 0.64 – – – – – –106 GSC 08608-00434 -0.09 – – B4V -0.20 – 0.12 –107 GSC 08608-00807 0.05 0.04 – B8V -0.12 – 0.16 –108 GSC 08608-00914 0.16 0.27 -0.76 B1V -0.28 -0.32 0.44 0.59109 GSC 08612-00331 0.14 0.09 – B2V -0.26 – 0.40 –110 GSC 08608-02412 -0.12 -0.05 -0.73 B3V -0.22 -0.23 0.11 0.15111 GSC 08612-00380 0.33 – – B3V -0.22 – 0.55 –112 GSC 08608-00239 0.31 0.37 – B0V -0.32 – 0.63 –MNRAS000
Table D1. continued.(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)No GSC ( B − V ) ( B − V ) ( U − B ) SpT&LC ( B − V ) ( B − V ) E ( B − V ) E ( B − V )Kh01 GCPD GCPD input spec. phot. avg. spec. phot. avg.APASS57 GSC 07123-00519 0.57 1.03 -0.15 – – -0.30 – 1.3358 GSC 08135-03248 -0.01 – – B2V -0.26 -0.22 0.24 0.2259 GSC 06565-01179 0.42 0.45 -0.67 B0V -0.32 -0.33 0.73 0.7860 GSC 07124-01160 1.00 -0.29 – – -0.34 – 1.3461 GSC 07120-02077 0.40 0.44 -0.73 B1V -0.28 -0.35 0.68 0.7962 GSC 06562-00688 0.03 0.11 – A3V 0.08 – -0.05 –63 GSC 05421-00568 0.06 -0.05 – – – – – –64 GSC 07659-01614 0.32 – – – – – –65 GSC 05438-00850 -0.09 -0.11 -0.39 B3V -0.22 -0.10 0.14 0.0166 GSC 07125-02097 0.21 0.45 -0.66 B0V -0.32 -0.33 0.53 0.7867 GSC 05435-00526 -0.13 -0.15 – B7IV -0.14 – 0.01 –68 GSC 07669-01154 0.73 – – – – – –69 GSC 07669-03714 -0.17 -0.07 -0.97 B2V -0.26 -0.31 0.08 0.2470 GSC 07139-02209 0.31 – – A0IV -0.02 – 0.33 –71 GSC 08151-01868 0.20 0.23 -0.60 B2V -0.26 -0.26 0.46 0.4972 GSC 08155-02404 0.17 0.27 -0.74 B1.5V -0.27 -0.31 0.43 0.5873 GSC 08164-01530 0.08 – – B1V -0.28 – 0.36 –74 GSC 08594-00620 -0.02 -0.05 -0.68 B3V -0.22 -0.22 0.20 0.1875 GSC 08165-00324 0.26 0.32 -0.49 B2V -0.26 -0.24 0.51 0.5676 GSC 08582-02609 0.71 – – – – – – –77 GSC 08591-00039 0.02 -0.07 -0.84 B1IV -0.28 -0.27 0.30 0.2078 GSC 07686-01898 0.15 0.19 – B7V -0.14 – 0.29 –79 GSC 08587-02162 0.09 0.13 -0.75 B2IV -0.26 -0.29 0.35 0.4080 GSC 08174-00235 0.26 0.29 -0.41 B5V -0.18 -0.21 0.44 0.5081 GSC 09196-00424 0.89 – – – – – –82 GSC 08588-02569 0.16 0.20 -0.57 B4V -0.20 -0.24 0.36 0.4483 GSC 08167-01520 0.20 0.25 -0.75 – – -0.32 – 0.5784 GSC 08593-01904 0.07 0.09 -0.66 B2V -0.26 -0.24 0.33 0.3385 GSC 08585-02212 0.11 0.08 -0.76 B1.5V -0.27 -0.28 0.38 0.3586 GSC 08593-00336 0.01 -0.01 – B8/9V -0.10 – 0.11 –87 GSC 07179-02573 0.00 – – B8V -0.12 – 0.11 –88 GSC 08593-02269 -0.05 -0.01 -0.73 B2.5V -0.24 -0.25 0.19 0.2589 GSC 08606-00053 0.06 – B4V -0.20 – 0.26 –90 GSC 08598-02245 0.11 0.19 -0.58 B3IV -0.22 -0.24 0.33 0.4391 GSC 08606-02020 0.64 0.66 -0.41 – – -0.30 – 0.9692 GSC 08610-03102 -0.05 – – B5V -0.18 – 0.14 –93 GSC 08603-00164 0.33 0.25 -0.63 – – -0.27 – 0.5294 GSC 08599-02357 0.07 0.12 -0.64 B5V -0.18 -0.24 0.25 0.3695 GSC 08611-01377 -0.09 -0.09 – B2V -0.26 -0.21 0.17 0.0996 GSC 08603-00677 0.59 0.61 – B7V -0.14 – 0.73 –97 GSC 08955-00160 0.04 – – B4V -0.20 – 0.24 –98 GSC 08943-00584 -0.02 0.02 – B5V -0.18 – 0.16 –99 GSC 08607-01004 1.51 – – – – – –100 GSC 08607-00285 0.43 0.52 -0.58 B1V -0.28 -0.32 0.71 0.84101 GSC 08604-00356 0.15 – – B6.5V -0.15 – 0.30 –102 GSC 08947-00809 0.14 0.09 -0.90 – – -0.32 – 0.41103 GSC 08943-02244 -0.05 0.08 -0.93 B0V -0.32 -0.33 0.26 0.41104 GSC 08943-00620 0.16 0.32 -0.75 B2V -0.26 -0.33 0.41 0.65105 GSC 08612-00975 0.64 – – – – – –106 GSC 08608-00434 -0.09 – – B4V -0.20 – 0.12 –107 GSC 08608-00807 0.05 0.04 – B8V -0.12 – 0.16 –108 GSC 08608-00914 0.16 0.27 -0.76 B1V -0.28 -0.32 0.44 0.59109 GSC 08612-00331 0.14 0.09 – B2V -0.26 – 0.40 –110 GSC 08608-02412 -0.12 -0.05 -0.73 B3V -0.22 -0.23 0.11 0.15111 GSC 08612-00380 0.33 – – B3V -0.22 – 0.55 –112 GSC 08608-00239 0.31 0.37 – B0V -0.32 – 0.63 –MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Table D1. continued.(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)No GSC ( B − V ) ( B − V ) ( U − B ) SpT&LC ( B − V ) ( B − V ) E ( B − V ) E ( B − V )Kh01 GCPD GCPD input spec. phot. avg. spec. phot. avg.APASS113 GSC 09397-00615 0.20 – – B5V -0.18 – 0.38 –114 GSC 08609-01016 0.29 0.28 -0.59 B1V -0.28 -0.27 0.57 0.55115 GSC 08605-01985 0.04 0.05 -0.48 B5V -0.18 -0.17 0.22 0.22116 GSC 08956-01223 0.11 0.10 -0.80 B7/8V -0.13 -0.29 0.23 0.37117 GSC 08613-01412 -0.03 -0.14 – B0V -0.32 – 0.29 –118 GSC 08613-00130 0.08 – – B5V -0.18 – 0.26 –119 GSC 08613-01744 0.70 – – – – – –120 GSC 08613-00147 0.57 0.48 -0.55 – – -0.30 – 0.78121 GSC 08957-02248 0.01 0.21 – B4V -0.20 – 0.21 –122 GSC 08609-00597 0.02 0.08 – B3V -0.22 – 0.24 –123 GSC 08622-01179 0.19 0.28 -0.76 – – -0.32 – 0.60124 GSC 08622-00429 0.26 0.34 -0.71 B2V -0.26 -0.32 0.52 0.66125 GSC 08626-00271 -0.09 0.06 -0.70 B1V -0.28 -0.25 0.20 0.31126 GSC 08957-03483 0.09 0.10 – – – – – –127 GSC 08961-01212 -0.03 0.10 – B2V -0.26 – 0.22 –128 GSC 08618-01375 0.09 0.11 – B8/9V -0.10 – 0.19 –129 GSC 08622-01758 0.08 – – B3V -0.22 – 0.30 –130 GSC 08622-01002 0.17 0.29 – A2V 0.05 – 0.12 –131 GSC 08618-01665 0.01 0.05 -0.90 B1V -0.28 -0.32 0.29 0.36132 GSC 08622-01017 0.12 0.13 -0.66 B2V -0.26 -0.25 0.37 0.38133 GSC 08965-01363 0.24 0.26 -0.54 B3IV -0.22 -0.24 0.46 0.50134 GSC 08969-00788 0.13 0.13 – – – – – –135 GSC 08958-02421 -0.01 – – B4V -0.20 – 0.19 0.16136 GSC 08623-02851 -0.19 0.48 – – – – – –137 GSC 08958-02242 -0.04 0.12 – – – – – –138 GSC 08619-01981 -0.04 -0.01 – – – – – –139 GSC 08627-00455 0.22 – – B5V -0.18 – 0.40 –140 GSC 08627-01249 0.15 0.23 -0.48 B2V -0.26 -0.22 0.41 0.45141 GSC 08958-02961 -0.02 – – B5V -0.18 -0.27 0.16 0.32142 GSC 08627-02220 0.17 0.19 -0.80 – – -0.31 – 0.50143 GSC 08958-03515 0.10 0.16 – – – – – –144 GSC 08627-02146 0.29 0.15 – A1V 0.01 – 0.28 –145 GSC 08958-00887 0.08 0.07 -0.85 B2V -0.26 -0.29 0.33 0.34146 GSC 08958-01376 -0.01 0.00 -0.78 B3V -0.22 -0.26 0.21 0.27147 GSC 08958-03463 0.05 0.30 – B5V -0.18 – 0.23 –148 GSC 08958-03384 0.28 0.23 – B8V -0.12 – 0.40 –149 GSC 08959-00482 0.21 0.16 -0.79 B2V -0.26 -0.30 0.47 0.46150 GSC 08967-00393 0.01 0.03 -0.73 B2V -0.26 -0.25 0.26 0.28151 GSC 08959-00488 0.24 0.26 -0.47 B5V -0.16 -0.22 0.40 0.48152 GSC 08628-00661 0.00 – – B5V -0.18 – 0.18 –153 GSC 08959-00863 0.03 0.12 -0.64 B1.5V -0.27 -0.24 0.30 0.36154 GSC 08959-00846 0.04 0.15 -0.73 B1V -0.28 -0.28 0.32 0.43155 GSC 08620-01856 -0.05 -0.05 -0.63 B7V -0.14 -0.20 0.10 0.15156 GSC 08959-02476 0.20 0.33 -0.39 O9.5V -0.32 -0.21 0.51 0.54157 GSC 08625-00369 -0.03 – – B7V -0.14 – 0.11 –158 GSC 08980-01582 0.87 0.70 -0.27 – – -0.26 – 0.96159 GSC 08972-00064 0.02 0.09 – – – -0.23 – 0.27160 GSC 08972-00932 -0.01 – – B9V -0.08 -0.18 0.08 0.16161 GSC 08642-01087 0.12 0.24 – – – – – –162 GSC 08973-00795 -0.01 0.06 -0.59 – – -0.21 – 0.27163 GSC 08973-00729 0.01 0.04 -0.73 – – -0.23 – 0.25164 GSC 08985-01836 0.15 0.22 – – – – – –165 GSC 08639-01611 -0.03 -0.01 – B2V -0.26 – 0.23 –166 GSC 08643-01679 0.10 0.08 -0.64 B3V -0.22 -0.23 0.32 0.31167 GSC 08973-01406 0.06 0.07 -0.62 – – -0.23 – 0.30168 GSC 08977-00310 -0.03 -0.02 -0.58 B2V -0.26 -0.20 0.23 0.19MNRAS , 1–46 (2017) Bernhard et al.
Table D1. continued.(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)No GSC ( B − V ) ( B − V ) ( U − B ) SpT&LC ( B − V ) ( B − V ) E ( B − V ) E ( B − V )Kh01 GCPD GCPD input spec. phot. avg. spec. phot. avg.APASS169 GSC 09234-02316 0.08 0.18 -0.77 B2V -0.26 -0.30 0.33 0.48170 GSC 08973-01861 0.07 0.10 -0.47 B5V -0.18 -0.19 0.25 0.29171 GSC 08977-00421 0.12 0.18 – B8V -0.12 – 0.23 –172 GSC 08978-01510 0.08 0.07 -0.50 – – -0.18 – 0.24173 GSC 08974-01031 0.03 0.06 -0.66 B4V -0.20 -0.22 0.23 0.27174 GSC 08974-00327 0.12 0.15 – B6V -0.16 – 0.28 –175 GSC 08982-00852 0.13 0.16 – – – – – –176 GSC 08641-01826 0.00 0.02 -0.35 B8/9IV -0.10 -0.12 0.10 0.14177 GSC 08974-00002 0.26 0.29 -0.39 B7V -0.14 -0.20 0.40 0.49178 GSC 08979-00623 0.10 – – B7V -0.14 -0.19 0.24 0.26179 GSC 08975-03998 0.02 – – B8V -0.12 – 0.13 –180 GSC 08975-00799 0.19 – – B3V -0.22 -0.17 0.41 0.42181 GSC 08988-02966 0.12 – – B8V -0.12 -0.14 0.24 0.35182 GSC 08992-01008 0.63 0.69 -0.40 B3V -0.22 -0.30 0.85 0.99183 GSC 08988-01196 0.11 0.09 -0.49 B3V -0.22 -0.20 0.33 0.31184 GSC 08989-02518 0.23 0.34 -0.27 B0V -0.32 -0.17 0.54 0.51185 GSC 09001-00465 0.08 – – B4V -0.20 – 0.28 –186 GSC 09245-01017 0.01 – – B6V -0.16 – 0.17 –187 GSC 08660-01131 0.29 0.32 -0.58 B1.5IV -0.27 -0.27 0.56 0.59188 GSC 08660-00731 0.27 0.31 -0.33 B2V -0.26 -0.19 0.53 0.50189 GSC 08652-02075 0.07 0.10 -0.21 B7V -0.14 -0.09 0.21 0.19190 GSC 08998-01018 0.03 0.04 -0.45 B5V -0.18 -0.16 0.21 0.20191 GSC 09245-00106 0.06 0.09 -0.89 B5V -0.18 -0.32 0.24 0.41192 GSC 08998-01663 0.16 0.19 -0.69 B0V -0.32 -0.27 0.47 0.47193 GSC 08990-00217 0.29 0.30 -0.65 B1V -0.28 -0.29 0.57 0.60194 GSC 08995-02904 0.17 0.25 -0.63 B2IV -0.26 -0.27 0.42 0.52195 GSC 07793-00222 -0.02 -0.08 – – – – – –196 GSC 09016-00519 -0.03 -0.03 – B3V -0.22 -0.21 0.19 0.15197 GSC 09008-04083 0.12 – – B9V -0.08 – 0.20 –198 GSC 08676-01771 0.03 0.10 – B2.5V -0.24 – 0.26 –199 GSC 09009-01997 0.30 0.36 -0.72 B0.5V -0.30 -0.33 0.60 0.66200 GSC 09009-02487 0.30 0.35 -0.74 B1V -0.28 -0.33 0.58 0.68201 GSC 09005-03448 0.27 0.24 -0.36 – – -0.18 – 0.42202 GSC 09005-03474 1.59 – – – – – –203 GSC 09013-01063 0.04 0.13 – – – – – –204 GSC 09006-04576 0.43 0.39 – – – – – –205 GSC 08691-03023 0.23 0.37 -0.42 – – -0.23 – 0.60206 GSC 08688-01283 0.04 0.11 – B9V -0.08 – 0.12 –207 GSC 09020-02147 0.58 0.56 -0.24 – – -0.22 – 0.78208 GSC 07821-02254 1.08 – – – – – –209 GSC 08305-02320 0.27 0.32 -0.02 B8V -0.12 -0.08 0.38 0.40210 GSC 09436-00541 0.08 0.13 – B8V -0.12 – 0.20 –211 GSC 08702-00469 -0.02 1.03 – – – – – –212 GSC 09033-02403 0.06 0.06 -0.63 B2V -0.26 -0.23 0.31 0.30213 GSC 08303-01041 0.28 0.29 -0.65 B2V -0.26 -0.29 0.53 0.58214 GSC 07847-00082 0.05 0.07 -0.28 B6V -0.16 -0.11 0.21 0.18215 GSC 08307-01059 0.01 0.07 – B7V -0.14 – 0.15 –216 GSC 09022-00605 0.11 0.09 -0.28 B6V -0.16 -0.12 0.27 0.21217 GSC 08701-00997 0.07 0.11 -0.51 B2V -0.26 -0.20 0.32 0.31218 GSC 08719-02158 -0.02 0.04 -0.40 B5V -0.18 -0.15 0.16 0.18219 GSC 08319-00698 0.07 0.04 -0.68 B2V -0.26 -0.24 0.32 0.28220 GSC 08719-00464 0.07 0.07 -0.36 B5V -0.18 -0.14 0.25 0.21221 GSC 08711-02092 0.08 0.08 -0.42 B5IV/V -0.18 -0.16 0.26 0.24222 GSC 08723-00042 0.01 0.04 -0.46 B3V -0.22 -0.17 0.23 0.20223 GSC 08715-01941 -0.02 0.00 -0.71 B2V -0.26 -0.24 0.24 0.24224 GSC 08712-02498 0.18 0.21 -0.52 B2.5IV -0.24 -0.23 0.42 0.44MNRAS000
Table D1. continued.(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)No GSC ( B − V ) ( B − V ) ( U − B ) SpT&LC ( B − V ) ( B − V ) E ( B − V ) E ( B − V )Kh01 GCPD GCPD input spec. phot. avg. spec. phot. avg.APASS169 GSC 09234-02316 0.08 0.18 -0.77 B2V -0.26 -0.30 0.33 0.48170 GSC 08973-01861 0.07 0.10 -0.47 B5V -0.18 -0.19 0.25 0.29171 GSC 08977-00421 0.12 0.18 – B8V -0.12 – 0.23 –172 GSC 08978-01510 0.08 0.07 -0.50 – – -0.18 – 0.24173 GSC 08974-01031 0.03 0.06 -0.66 B4V -0.20 -0.22 0.23 0.27174 GSC 08974-00327 0.12 0.15 – B6V -0.16 – 0.28 –175 GSC 08982-00852 0.13 0.16 – – – – – –176 GSC 08641-01826 0.00 0.02 -0.35 B8/9IV -0.10 -0.12 0.10 0.14177 GSC 08974-00002 0.26 0.29 -0.39 B7V -0.14 -0.20 0.40 0.49178 GSC 08979-00623 0.10 – – B7V -0.14 -0.19 0.24 0.26179 GSC 08975-03998 0.02 – – B8V -0.12 – 0.13 –180 GSC 08975-00799 0.19 – – B3V -0.22 -0.17 0.41 0.42181 GSC 08988-02966 0.12 – – B8V -0.12 -0.14 0.24 0.35182 GSC 08992-01008 0.63 0.69 -0.40 B3V -0.22 -0.30 0.85 0.99183 GSC 08988-01196 0.11 0.09 -0.49 B3V -0.22 -0.20 0.33 0.31184 GSC 08989-02518 0.23 0.34 -0.27 B0V -0.32 -0.17 0.54 0.51185 GSC 09001-00465 0.08 – – B4V -0.20 – 0.28 –186 GSC 09245-01017 0.01 – – B6V -0.16 – 0.17 –187 GSC 08660-01131 0.29 0.32 -0.58 B1.5IV -0.27 -0.27 0.56 0.59188 GSC 08660-00731 0.27 0.31 -0.33 B2V -0.26 -0.19 0.53 0.50189 GSC 08652-02075 0.07 0.10 -0.21 B7V -0.14 -0.09 0.21 0.19190 GSC 08998-01018 0.03 0.04 -0.45 B5V -0.18 -0.16 0.21 0.20191 GSC 09245-00106 0.06 0.09 -0.89 B5V -0.18 -0.32 0.24 0.41192 GSC 08998-01663 0.16 0.19 -0.69 B0V -0.32 -0.27 0.47 0.47193 GSC 08990-00217 0.29 0.30 -0.65 B1V -0.28 -0.29 0.57 0.60194 GSC 08995-02904 0.17 0.25 -0.63 B2IV -0.26 -0.27 0.42 0.52195 GSC 07793-00222 -0.02 -0.08 – – – – – –196 GSC 09016-00519 -0.03 -0.03 – B3V -0.22 -0.21 0.19 0.15197 GSC 09008-04083 0.12 – – B9V -0.08 – 0.20 –198 GSC 08676-01771 0.03 0.10 – B2.5V -0.24 – 0.26 –199 GSC 09009-01997 0.30 0.36 -0.72 B0.5V -0.30 -0.33 0.60 0.66200 GSC 09009-02487 0.30 0.35 -0.74 B1V -0.28 -0.33 0.58 0.68201 GSC 09005-03448 0.27 0.24 -0.36 – – -0.18 – 0.42202 GSC 09005-03474 1.59 – – – – – –203 GSC 09013-01063 0.04 0.13 – – – – – –204 GSC 09006-04576 0.43 0.39 – – – – – –205 GSC 08691-03023 0.23 0.37 -0.42 – – -0.23 – 0.60206 GSC 08688-01283 0.04 0.11 – B9V -0.08 – 0.12 –207 GSC 09020-02147 0.58 0.56 -0.24 – – -0.22 – 0.78208 GSC 07821-02254 1.08 – – – – – –209 GSC 08305-02320 0.27 0.32 -0.02 B8V -0.12 -0.08 0.38 0.40210 GSC 09436-00541 0.08 0.13 – B8V -0.12 – 0.20 –211 GSC 08702-00469 -0.02 1.03 – – – – – –212 GSC 09033-02403 0.06 0.06 -0.63 B2V -0.26 -0.23 0.31 0.30213 GSC 08303-01041 0.28 0.29 -0.65 B2V -0.26 -0.29 0.53 0.58214 GSC 07847-00082 0.05 0.07 -0.28 B6V -0.16 -0.11 0.21 0.18215 GSC 08307-01059 0.01 0.07 – B7V -0.14 – 0.15 –216 GSC 09022-00605 0.11 0.09 -0.28 B6V -0.16 -0.12 0.27 0.21217 GSC 08701-00997 0.07 0.11 -0.51 B2V -0.26 -0.20 0.32 0.31218 GSC 08719-02158 -0.02 0.04 -0.40 B5V -0.18 -0.15 0.16 0.18219 GSC 08319-00698 0.07 0.04 -0.68 B2V -0.26 -0.24 0.32 0.28220 GSC 08719-00464 0.07 0.07 -0.36 B5V -0.18 -0.14 0.25 0.21221 GSC 08711-02092 0.08 0.08 -0.42 B5IV/V -0.18 -0.16 0.26 0.24222 GSC 08723-00042 0.01 0.04 -0.46 B3V -0.22 -0.17 0.23 0.20223 GSC 08715-01941 -0.02 0.00 -0.71 B2V -0.26 -0.24 0.24 0.24224 GSC 08712-02498 0.18 0.21 -0.52 B2.5IV -0.24 -0.23 0.42 0.44MNRAS000 , 1–46 (2017) n investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data Table D1. continued.(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)No GSC ( B − V ) ( B − V ) ( U − B ) SpT&LC ( B − V ) ( B − V ) E ( B − V ) E ( B − V )Kh01 GCPD GCPD input spec. phot. avg. spec. phot. avg.APASS225 GSC 08325-05810 0.26 0.29 -0.56 B1V -0.28 -0.26 0.54 0.55226 GSC 09042-01527 -0.11 -0.08 -0.56 B7V -0.14 -0.17 0.03 0.09227 GSC 08337-00341 0.05 0.11 -0.20 B6V -0.16 -0.09 0.21 0.20228 GSC 08325-00916 0.30 0.30 – A2V 0.05 – 0.25 –229 GSC 08330-05153 -0.01 – – B3V -0.22 – 0.21 –230 GSC 08338-02080 0.16 0.18 -0.70 B2V -0.26 -0.28 0.41 0.46231 GSC 08734-02077 0.02 0.06 0.00 – – -0.01 – 0.07232 GSC 07872-00681 0.17 0.22 -0.76 – – -0.30 – 0.51233 GSC 07872-00390 0.13 0.14 -0.71 B1IV -0.28 -0.27 0.41 0.40234 GSC 08328-00373 0.30 0.36 -0.36 B3V -0.22 -0.21 0.52 0.55235 GSC 07878-00246 0.05 0.08 -0.54 B2V -0.26 -0.19 0.31 0.26236 GSC 08345-03046 0.05 – – B8V -0.12 – 0.17 –237 GSC 07374-00838 0.72 0.80 -0.27 B0.5V -0.30 -0.28 1.02 1.08238 GSC 07366-00860 0.72 0.91 0.04 – – -0.21 – 1.12239 GSC 08341-00889 0.03 0.07 -0.41 B5V -0.18 -0.15 0.21 0.22240 GSC 07375-00048 0.20 – – B3IV -0.22 – 0.42 –241 GSC 08342-00052 0.02 0.09 – B9V -0.08 – 0.10 –242 GSC 07384-00247 0.67 0.62 -0.31 – – -0.25 – 0.87243 GSC 08342-01635 -0.02 -0.02 -0.61 B2V -0.26 -0.22 0.23 0.21244 GSC 06835-00151 0.30 0.57 – – – – – –245 GSC 06839-00611 0.56 0.74 -0.22 – – -0.25 – 0.99246 GSC 07889-01252 0.13 – – B7/8V -0.13 – 0.26 –247 GSC 07385-01338 0.20 0.23 -0.50 B8V -0.12 -0.23 0.31 0.45248 GSC 07886-02848 0.00 0.02 -0.58 B1.5V -0.27 -0.20 0.27 0.22249 GSC 06853-01718 – – – – – – –250 GSC 06853-02519 0.49 0.53 -0.51 – – -0.30 – 0.83251 GSC 06841-01725 0.57 0.97 – – – – – –252 GSC 06846-01106 0.75 0.87 -0.20 – – -0.28 – 1.15253 GSC 07399-01124 0.06 – – B4V -0.20 – 0.26 –254 GSC 06263-03157 0.08 – – B3V -0.22 -0.16 0.30 0.23255 GSC 07399-01226 0.01 – – B5V -0.18 – 0.19 –256 GSC 06272-02199 0.36 0.38 -0.29 B5V -0.18 -0.19 0.54 0.57257 GSC 06268-02490 0.31 0.35 -0.33 B2V -0.26 -0.20 0.57 0.55258 GSC 06276-00317 -0.03 – – B8V -0.12 – 0.09 –259 GSC 06851-02063 0.11 – – B7V -0.14 – 0.25 –260 GSC 06847-02930 0.47 0.64 -0.46 – – -0.31 – 0.95261 GSC 06851-04189 -0.02 – – B5V -0.18 – 0.16 –262 GSC 06268-00943 0.20 0.26 – B7V -0.14 – 0.34 –263 GSC 06847-02073 0.05 0.08 -0.64 B5V -0.18 -0.23 0.23 0.31264 GSC 06272-00394 0.16 0.17 – B5IV -0.18 – 0.34 –265 GSC 07404-05201 -0.08 -0.11 -0.60 B3V -0.22 -0.18 0.14 0.07266 GSC 06269-02592 0.77 0.78 -0.10 – – -0.22 – 1.00267 GSC 06274-00902 0.34 0.37 – A0V -0.02 – 0.36 –268 GSC 07909-02656 -0.10 0.00 – B8V -0.12 – 0.02 –269 GSC 05703-02553 0.18 0.19 -0.40 B3V -0.22 -0.18 0.40 0.37270 GSC 05124-01543 1.18 0.77 – B5V -0.18 – 1.36 –271 GSC 05703-01526 0.29 0.32 – – – – – –272 GSC 06275-00943 0.08 0.08 -0.28 B2IV -0.26 -0.11 0.34 0.19273 GSC 05692-01642 0.37 0.39 – B3V -0.22 – 0.59 –274 GSC 05125-02006 0.34 0.26 – B3V -0.22 – 0.56 –275 GSC 00456-00461 0.37 0.44 -0.04 B8V -0.12 -0.12 0.48 0.56276 GSC 05693-07523 0.10 – – – – – – –277 GSC 05126-03377 0.13 0.35 – – – – – –278 GSC 05701-00964 0.27 0.25 – B4V -0.20 -0.17 0.47 0.46279 GSC 01026-02065 0.51 0.57 -0.29 B2.5V -0.24 -0.23 0.74 0.82280 GSC 06289-02980 0.14 0.16 -0.30 B9V -0.08 -0.14 0.22 0.30MNRAS , 1–46 (2017) Bernhard et al.
Table D1. continued.(1) (2) (3) (4) (5) (6) (7) (8) (9) (10)No GSC ( B − V ) ( B − V ) ( U − B ) SpT&LC ( B − V ) ( B − V ) E ( B − V ) E ( B − V )Kh01 GCPD GCPD input spec. phot. avg. spec. phot. avg.APASS281 GSC 05123-00145 0.43 0.47 – B3V -0.22 – 0.65 –282 GSC 00463-02825 0.45 0.61 – B2V -0.26 – 0.70 0.65283 GSC 05131-01423 0.10 0.09 -0.41 B2V -0.26 -0.16 0.36 0.25284 GSC 02129-00864 0.57 0.54 – – – – – –285 GSC 05149-01177 0.13 – – B8V -0.12 – 0.24 –286 GSC 01645-00281 -0.12 – – – – – – –287 GSC 01124-01184 -0.05 -0.03 – B8V -0.12 – 0.07 –MNRAS000