S-PLUS: LEnticular Galaxies in Stripe 82
A. Cortesi, K. Saha, F.Ferrari, G. Lucatelli, C. Mendes de Oliveira, S. Dhiwar, C. R. Bom, L. O. Dias
MMNRAS , 1–3 (2021) Preprint 9 February 2021 Compiled using MNRAS L A TEX style file v3.0
S-PLUS: LEnticular Galaxies in Stripe 82
A. Cortesi (cid:63) , K. Saha , F.Ferrari , G. Lucatelli , C. Mendes de Oliveira , S. Dhiwar ,C. R. Bom , L. O. Dias Observat´orio do Valongo, Ladeira (OV) Inter-University Centre for Astronomy and Astrophysics (IUCAA) Universidade Federal do Rio Grande (FURG) Universidade de S˜ao Paulo Brazilian Center for Physics Research (CBPF)
Accepted in Anais da Academia Brasileira de Ciencias
ABSTRACT
This work is a Brazilian-Indian collaboration. It aims at investigating the structuralproperties of Lenticular galaxies in the Stripe 82 using a combination of S-PLUS(Southern Photometric Local Universe Survey) and SDSS data. S-PLUS is a noveloptical multi-wavelength survey which will cover nearly 8000 square degrees of theSouthern hemisphere in the next years and the first data release covers the Stripe 82area. The morphological classification and study of the galaxies’ stellar population willbe performed combining the Bayesian Spectral type (from BPZ) and Morfometryka(MFMTK) parameters. BPZ and MFMTK are two complementary techniques, sincethe first one determines the most likely stellar population of a galaxy, in order toobtain its photometric redshift (phot-z), and the second one recovers non-parametricmorphological quantities, such as asymmetries and concentration. The combination ofthe two methods allows us to explore the correlation between galaxies shapes (smooth,with spiral arms, etc.) and their stellar contents (old or young population). The pre-liminary results, presented in this work, show how this new data set opens a newwindow on our understanding of the nearby universe.
Key words: galaxies: elliptical and lenticular, cD, galaxies: individual: NGC 1023,galaxies: kinematics and dynamics.
Lenticular galaxies have been largely studied, since whenthey have been first classified by Edwin Hubble Hubble(1936), as the missing link between elliptical and spiralgalaxies. S0s or lenticular galaxies present, in fact, an hy-brid structure, showing a prominent disk, but with no signsof spiral arms. The presence of the disk suggests that theirkinematics is rotationally supported Cortesi et al. (2013a,b),as found for spiral galaxies Merrett et al. (2003). Ellipti-cal galaxies, on the contrary, are pressure supported sys-tems, as a result of their formation histories, which com-prise a sequence of major and minor mergers Bournaud,Jog & Combes (2005). Moreover, lenticular galaxies aremore frequently found in denser regions of galaxy clus-ters Dressler (1980) and their frequency increases towardslow redshifts Dressler et al. (1997). Considering that thisis an opposite trend to that of spiral galaxies, it has beenfirst hypothesised that S0 galaxies may be the end prod- (cid:63)
E-mail: [email protected] uct of spiral galaxies whose gas was gently stripped orconsumed. Such evolutionary path would require the inter-play between the galaxy and the surrounding environmentto cease star formation and remove the spiral arms. Yet,field lenticular galaxies exist. At the present moment, sev-eral mechanisms have been pointed out as possible ways tocreate lenticular galaxies: minor mergers Bournaud, Jog &Combes (2005), major mergers under specific initial condi-tions Eliche-Moral et al. (2018), AGN feedback or/and secu-lar evolution Mishra, Wadadekar & Barway (2018), and it isbecoming more popular the idea that the S0 class is actuallya compilation of objects that formed through very differentpaths and just happen to have similar appearances. Partof the problem stands on the difficulty of visually identify-ing lenticular galaxies. In fact, there is not a consensus onthe morphological characteristics of lenticular galaxies andthey can, in general, be easily misclassified due to the vagueappearence of spiral arms, and not trivial determination ofthe presence of a disk, from a purely photometric approach.Large spectroscopic surveys, on the other side, often coversonly the central part of a galaxy, i.e. the region where the © a r X i v : . [ a s t r o - ph . GA ] F e b Cortesi et al. bulge dominates, again making it hard to separate ellipticalgalaxies, from lenticular galaxies with large bulge-over-totallight ratio. Multi-wavelength surveys (as S-PLUS Mendes deOliveira et al. (2019)) open a new window on galaxy classifi-cation, combining the possibility of studying the variation ofmorphological parameters with wavelengths and recoveringthe galaxy stellar population. We present preliminary resultsof this approach, using the S-PLUS first data release , andwe describe new methods to identify lenticular galaxies. S-PLUS (Southern Photometric Local Universe Survey) isan astronomical facility in Chile (Cerro Pachon), dedicatedto mapping the observable sky in 7 narrow-band filters and5 broad-band (ugriz) filters in the optical region. The 0.86mmirror of the T80-South telescope, combined with a field ofview of 1.4 square degrees and an 85 Mega-pixel camera, isproducing high-quality images and a unique spectral reso-lution for millions of objects over several thousand squaredegrees. Together with its twin observatory in the northernhemisphere, the T80-North, its sister survey J-PLUS, willcast the first light on a multi-colour Universe, on about halfof the extragalactic sky. This multi-purpose astrophysicalsurvey in the southern hemisphere started in 2016. Duringthe next 3-4 years it will observe more than 8,000 squaredegrees (1/5 of the whole sky), covering the entire visibleregion of the electromagnetic spectrum (3500 A to 10,000A). Figure 1 and 2 show the area covered in the sky and theJavalambre filter system used by S-PLUS.Galaxy morphologies vary with wavelength, since dif-ferent stellar populations present different colours. In gen-eral, star forming galaxies have a lower bulge-to-total (
B/T )light ratio than quiescent ones Morselli et al. (2017). Weuse
Morfometryka
Ferrari, de Carvalho & Trevisan (2015)(MFMTK) to compute galaxies’ non-parametric morphome-tric parameters, in particular we recover the concentration(C1) and the entropy (H). The concentration is defined asthe ratio of the radii containing some fraction of the totallight inside the Petrosian Region (2Rp): C = log (cid:16) R R (cid:17) , where R f is the radius that contains a fraction of f %. En-tropy is defined as: H ( I ) = − n (cid:88) i p ( I i ) ln[ p ( I i )] /H max , where p is the probability of the occurence of the intensity I i and H max is the maximum entropy, which is for an homoge-neous distribution (e.g. p = 1 /n ). For the early type galaxiesthe concentration is nearly constant with wavelength, whileit increases for redder wavelengths, in the case of the spi-ral galaxies. Another feature is that homogeneous systems(with less concentrated light distributions, such as disks orextended galaxies) have higher entropies than systems withmore concentrated light distributions (ellipticals, bulge dom-inated, compacted, etc.). Finally, we use the Bayesian Pho-tometric redshifts (BPZ) Molino et al. (2014) method to https://datalab.noao.edu/splus/ S-PLUS Survey Area
S-PLUSATLASVVVVPHAS DECALDESKIDSGAMMA
Figure 1.
Diagram showing some of the most important opticaland near-infrared surveys in the Southern Hemisphere (we omitthe surveys SkyMapper, Gaia and LSST that cover the entirehemisphere or sky). For the optical surveys: ATLAS is shown inhatched green, VPHAS+ is the pink rectangular contour over theBulge and Disk of the Galaxy, DECAL is in hatched black, DESis shown in blue, KiDS in yellow, and GAMA in bright green. Theonly near-infrared survey displayed is VISTA-VVV, a rectanglewith light gray contours over the Galactic disk. Dark red showsthe area covered by S-PLUS. The broken black line representsthe ecliptic. The figure is taken from Mendes de Oliveira et al. (2019).
Figure 2.
The Javalambre 12-filter system used by S-PLUS. They-axis shows the total efficiency of the filters, obtained throughthe multiplication of the average transmission curves, the CCDefficiency, and the mirror reflectivity curves. Different filters arecoloured according to the labels on the right-side panel. The figureis taken from Mendes de Oliveira et al. (2019). obtain the galaxy bayesian spectral type, by identifying thegalaxy template model that optimises the redshift determi-nation, for more details see Molino et al. (2020).
The top panel of Figure 3 shows the distribution of thegalaxies in the H − C MNRAS000
The top panel of Figure 3 shows the distribution of thegalaxies in the H − C MNRAS000 , 1–3 (2021) -PLUS: LEnticular Galaxies in Stripe 82 their morphological type Nair & Abraham (2010). The T-Type parameter value is lower than − − H − C et al. (2020). The galaxies’ templates are defined as fol-lows: from T1 to T4 is a spectral energy distribution (SED)typical of elliptical galaxies, T5 is for ES0 galaxies, fromT6 to T14 are spiral galaxies templates (barred and un-barred). Again, the morphometric parameters allow us todivide galaxies into passive (early-type galaxies) and starforming (late-type galaxies). Interestingly, several T1 galax-ies lie in the part of the plot populated by spiral galaxies,and some galaxies characterised by a spiral-like galaxy tem-plates fall in the upper area of the plot, where we expectto find early type galaxies. This finding shows that galaxies’morphology and stellar content are not always as expected:the universe present blue ellipticals and red spirals Strateva et al. (2001). S-PLUS data set allows to recover both thesequantities and map the galaxy distribution in the local uni-verse. In this work we present preliminary results of the studyof galaxy morphology and stellar population properties ob-tained using data of the S-PLUS survey. We show howthe parameters recovered with MFMTK allow to performa galaxy morphological classification and we suggest a wayto identify S0 galaxies, combining such parameters with anovel method based on the study of the curvature of thegalaxies’ surface light profile Lucatelli & Ferrari (2019). TheS-PLUS data set, given its unique combination of narrowand broad band filters, allows the estimation of the galaxymost probable stellar template, together with the definitionof its morphometric parameters. This study extends fromobservational astronomy, to theory and computational anal-ysis; it comprises researchers from Brazil and India and it isopen to a world-wide collaboration. With its 0.86 cm diam-eter, S-PLUS proves the importance of small telescopes inthe advance of astronomical knowledge. Several other smalltelescopes exist in the BRICS countries. We conclude en-couraging a dialogue among these telescope users, sharingtechnical and scientific knowledge.
AC acknowledges support from PNPD/CAPES. : : : : : : : : : : : : : : : : : : C ¡ ¡ T ¡ T y p e : : : : : : : : : : : : : : : : : : C T b Figure 3.
Entropy versus concentration parameters, estimatedusing MFMTK, for a sample of 925 galaxies, colour coded ac-cording to their morphological T-Type, top panel, and accordingto their bayesian spectral templates, bottom panel. See text formore details.
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