S. Antoniucci

Accretion and ejection properties of embedded protostars: the case of HH26, HH34, and HH46 IRS

Aims. We present the results of a spectroscopic analysis of three young embedded sources (HH26 IRS, HH34 IRS, and HH46 IRS) belonging to different star-forming regions and displaying well-developed jet structures. The aim is to investigate the source accretion and ejection properties and their connection. Methods. We used VLT-ISAAC near-IR medium resolution (R ∼ 9000) spectra (H and K bands) to derive, in a self-consistent way, parameters like the star luminosity, accretion luminosity, and the mass accretion rate. Mass ejection rates have also been estimated from analysing different emission features. Results. The spectra present several emission lines but no photospheric features in absorption, indicating a large veiling in both the H and K bands. In addition to features commonly observed in jet driving sources ([Fe ii], H2 ,H i, CO), we detect a number of emission lines due to permitted atomic transitions, such as Na i and Ti i that are only 2−5 times weaker than the Brγ line. Some of these features remain unidentified. Emission from Na i 2.2 µm doublet is observed along with CO(2−0) band-head emission, indicating a common origin in an inner gaseous disc heated by accretion. We find that accretion provides about 50% and 80% of the bolometric luminosity

Probing the embedded YSOs of the R CrA region through VLT-ISAAC spectroscopy ,

Near IR spectra at low (R ∼ 800) and medium (R ∼ 9000) resolution, obtained with ISAAC at VLT, have been used to pose constraints on the evolutionary state and accretion properties of a sample of five embedded YSOs located in the R CrA core. This sample includes three Class I sources (HH100 IR, IRS2 and IRS5), and two sources with NIR excesses (IRS6 and IRS3). IRS5 and IRS6 have been discovered to be binaries with a separation between the two components of 78 and 97 AU, respectively. Absorption lines, typical of late-type photospheres, have been detected in the medium resolution spectra of all the observed targets, including HH 100 IR and IRS2 which have high values of infrared continuum veiling (r K = 6 and 3, respectively). These two sources also present low resolution spectra rich in emission lines (HI, CO and plenty of other permitted lines from neutral atoms) likely originating in the disk-star-wind connected regions. Among the features observed in HH100 IR and IRS2, Na I at 2.205 μm and CO at 2.3 μm, which are more commonly used for stellar classification, are detected in emission instead of absorption. Several strong photospheric lines which lie around 2.12 and 2.23 μm and whose ratio is sensitive to both effective temperature and gravity are proposed as independent diagnostic tools for this type of sources. We derived spectral types, veiling and stellar luminosity for the five observed sources, which in turn have been used to infer their mass (ranging between 0.3-1.2 M ○. ) and age (between 10 5 and 10 6 yr) adopting pre-main sequence evolutionary tracks. We find that in HH100 IR and IRS2 most of the bolometric luminosity is due to accretion (L acc /L bol ∼ 0.8 and 0.6 respectively), while the other three investigated sources, including the Class I object IRS5a, present low accretion activity (L acc /L bol < 0.2). Mass accretion rates of the order of 2 x 10 -6 and 3 x 10 -7 M ○. yr -1 are derived for HH100 IR and IRS2, respectively, i.e. higher by an order of magnitude than the average values derived for T Tauri stars. We observe a general correlation between the accretion luminosity, the IR veiling and the emission line activity of the sources. In particular, we find that the correlation between L acc and L Brγ , previously reported for optical T Tauri stars, can be extended to the embedded sources, up to at least one order of magnitude larger line luminosity. A correlation between the accretion activity and the spectral energy distribution slope is recognizable with the notable exception of IRS5a. Our analysis therefore shows how the definition of the evolutionary stage of deeply embedded YSOs by means of IR colors needs to be refined.

NEAR-INFRARED SPECTROSCOPIC MONITORING OF EXOR VARIABLES: FIRST RESULTS*

We present low-resolution spectroscopy in the near-IR (0.8-2.5 μm) of the EXor variables. These are the initial results (obtained during the period 2007-2008) from a long-term photometric and spectroscopic program aimed to study the variability in the accretion processes of pre-main-sequence stars, by correlating the continuum fluctuations with the spectroscopic properties. Eight sources have been observed in different epochs, for a total of 25 acquired spectra. EXor spectra show a wide variety of emission features dominated by H I recombination (Paschen and Brackett series). We have investigated whether line and continuum variability could be due to a variable extinction, but such a hypothesis is applicable only to the peculiar source PV Cep. By comparing the observed spectra with a wind model, mass loss rates in the range (2-10) × 10–8 M ☉ yr–1 are derived, along with other wind parameters. Consistent results are also obtained by assuming that H I lines are due to accretion. A CO overtone is also detected in the majority of the sources both in absorption and in emission. It appears to come from regions more compact than winds, likely the stellar photosphere (when in absorption) and the circumstellar disk (when in emission). Na I and Ca I IR lines behave as the CO does, thus they are thought to arise in the same locations. For some targets multiple spectra correspond to different activity stages of the source. Those exhibiting the largest continuum variation at 2 μm (ΔK 1 mag) present a significant line flux fading during the continuum declining phases. In particular, CO absorption (emission) appears associated with inactive (active) stages, respectively.

POISSON project - I. Emission lines as accretion tracers in young stellar objects: results from observations of Chamaeleon I and II sources

Context. We present the results of the analysis of low-resolution optical-near IR spectroscopy (0.6–2.4 μm) of a sample (47 sources) of Class I and Class II young stellar objects in the Chamaeleon I and II star-forming clouds. These data are part of the POISSON project (Protostellar Optical-Infrared Spectral Survey On NTT). Aims. The aim of the observations is to determine the accretion luminosity (Lacc) and mass accretion rate ( u Macc) of the sources through the analysis of the detected emission features. Taking advantage of the wide wavelength range covered by our spectra, we also aim at verifying the reliability and consistency of the existing empirical relationships connecting emission line luminosity and Lacc. Methods. We employ five different tracers ([O i] λ6300, Hα ,C aii λ8542, Paβ ,a nd Brγ) to derive the accretion luminosity, and critically discuss the various determinations in the light of the source properties. Results. The tracers provide Lacc values characterised by different scatters when plotted as a function of L∗ .T he Brγ relation appears to be the most reliable, because it gives the minimum dispersion of Lacc over the entire range of L∗, whereas the other tracers, in particular Hα, provide much more scattered Lacc results, which are not expected for the homogeneous sample of targets we are observing. The direct comparison between Lacc(Brγ) and the accretion luminosity obtained from the other four tracers also shows systematic differences in the results provided by the empirical relationships. These may probably be ascribed to different excitation mechanisms that contribute to the line emission, which may vary between our sample and those where the relationships have been calibrated, which were mostly based on observations in Taurus. Adopting the accretion luminosities estimates derived from the Brγ line, we infer Lacc in the range 0.1 L∗–1 L∗ for all sources, and u −

The Herschel HIFI water line survey in the low-mass proto-stellar outflow L1448

Aims. As part of the WISH (Water In Star-forming regions with Herschel) key project, systematic observations of H2O transitions in young outflows are being carried out with the aim of understanding the role of water in shock chemistry and its physical and dynamical properties. We report on the observations of several ortho-and para-H2O lines performed with the HIFI instrument toward two bright shock spots (R4 and B2) along the outflow driven by the L1448 low-mass proto-stellar system, located in the Perseus cloud. These data are used to identify the physical conditions giving rise to the H2O emission and to infer any dependence on velocity. Methods. We used a large velocity gradient (LVG) analysis to derive the main physical parameters of the emitting regions, namely n(H-2), T-kin, N(H2O) and emitting-region size. We compared these with other main shock tracers, such as CO, SiO and H-2 and with shock models available in the literature. Results. These observations provide evidence that the observed water lines probe a warm (T-kin similar to 400-600 K) and very dense (n similar to 10(6)-10(7) cm(-3)) gas that is not traced by other molecules, such as low-J CO and SiO, but is traced by mid-IR H-2 emission. In particular, H2O shows strong differences with SiO in the excitation conditions and in the line profiles in the two observed shocked positions, pointing to chemical variations across the various velocity regimes and chemical evolution in the different shock spots. Physical and kinematical differences can be seen at the two shocked positions. At the R4 position, two velocity components with different excitation can be distinguished, of which the component at higher velocity (R4-HV) is less extended and less dense than the low velocity component (R4-LV). H2O column densities of about 2 x 10(13) and 4 x 10(14) cm(-2) were derived for the R4-LV and the R4-HV components, respectively. The conditions inferred for the B2 position are similar to those of the R4-HV component, with H2O column density in the range 10(14)-5 x 10(14) cm(-2), corresponding to H2O/H-2 abundances in the range 0.5-1 x 10(-5). The observed line ratios and the derived physical conditions seem to be more consistent with excitation in a low-velocity J-type shock with strong compression rather than in a stationary C-shock, although none of these stationary models seems able to reproduce the whole characteristics of the observed emission.

On the Nature of EXor Accretion Events: An Infrequent Manifestation of a Common Phenomenology?

We present the results of a comparison between classical and newly identified EXor based on literature data and aimed at recognizing possible differences or similarities between the categories. Optical and near-IR two-color diagrams, modalities of fluctuations, and derived values of the mass accretion rates are indicative of strong similarities between the two samples. We demonstrate how the difference between the outburst and the quiescence spectral energy distribution of all EXor can be well fitted with a single blackbody, as if an additional thermal component appears during the outbursting phase. Temperatures of this additional component span between 1000 and 4500 K, while the radii of the emitting regions (assumed to be a uniform disk) span between 0.01 and 0.1 AU, sizes typical of the inner portions of the circumstellar disk. Spots persisting up to 50% of the outburst duration, not exceeding 10% of the stellar surface, and with temperatures compatible with the EXor mass accretion rates, are able to account for both the appearance of the additional thermal component and the dust sublimation in the inner structures of the disk. We also compare the EXor events with the most significant color and magnitude fluctuations of active T Tauri stars finding that (1) burst accretion phenomena should also be important for this latter class and (2) EXor events could be more frequent than those accidentally discovered. A remarkable case is that of the source V2493 Cyg, a T Tauri star recently identified as a strong outbursting object: New optical and near-IR photometric and spectroscopic data are presented in an attempt to clarify its EXor or FUor nature.

POISSON project - II. A multi-wavelength spectroscopic and photometric survey of young protostars in L 1641

Context. Characterising stellar and circumstellar properties of embedded young stellar objects (YSOs) is mandatory for understanding the early stages of the stellar evolution. This task requires the combination of both spectroscopy and photometry, covering the widest possible wavelength range, to disentangle the various protostellar components and activities. Aims. As part of the POISSON project (Protostellar Optical-Infrared Spectral Survey On NTT), we present a multi-wavelength spectroscopic and photometric investigation of embedded YSOs in L 1641, aimed to derive the stellar parameters and evolutionary stages and to infer their accretion properties. Methods. Our multi-wavelength database includes low-resolution optical-IR spectra from the NTT and Spitzer (0.6−40 μm) and photometric data covering a spectral range from 0.4 to 1100 μm, which allow us to construct the YSOs spectral energy distributions (SEDs) and to infer the main stellar parameters (visual extinction, spectral type, accretion, stellar, bolometric luminosity, mass accretion, and ejection rates). Results. The NTT optical-NIR spectra are rich in emission lines, which are mostly associated with YSO accretion, ejection, and chromospheric activities. A few emission lines, prominent ice (H2 Oa nd CO 2), and amorphous silicate absorption features have also been detected in the Spitzer spectra. The SED analysis allows us to group our 27 YSOs into nine Class I, eleven Flat, and seven Class II objects. However, on the basis of the derived stellar properties, only six Class I YSOs have an age of ∼10 5 yr, while the others are older (5 × 10 5 −10 6 yr), and, among the Flat sources, three out of eleven are more evolved objects (5 × 10 6 −10 7 yr), indicating that geometrical effects can significantly modify the SED shapes. Inferred mass accretion rates ( u Macc) show a wide range of values � � ) 3 6

The outburst of an embedded low-mass YSO in L1641

Context. Strong outbursts in very young and embedded protostars are rare and not yet fully understood. They are believed to originate from an increase in the mass accretion rate (M acc ) onto the source. Aims. We report the discovery of a strong outburst in a low-mass embedded young stellar object (YSO), namely 2MASS-J05424848-0816347 or [CTF93]216-2, as well as its photometric and spectroscopic follow-up. Methods. Using near- to mid-IR photometry and NIR low-resolution spectroscopy, we monitor the outburst, deriving its magnitude, duration, as well as the enhanced accretion luminosity and mass accretion rate. Results. [CTF93]216-2 increased in brightness by ~4.6, 4.0, 3.8, and 1.9 mag in the J, H, K s bands and at 24 μm, respectively, corresponding to an L bol increase of ~20 L ⊙ . Its early spectrum, probably taken soon after the outburst, displays a steep almost featureless continuum, with strong CO band heads and H 2 O broad-band absorption features, and Brγ line in emission. A later spectrum reveals more absorption features, allowing us to estimate T eff ~ 3200 K, M* ~ 0.25 M ⊙ , and M acc ~ 1.2 × 10 -6 M ⊙ yr -1 . This makes it one of the lowest mass YSOs with a strong outburst so far discovered.

X-shooter spectroscopy of young stellar objects in Lupus - Accretion properties of class II and transitional objects

The mass accretion rate, Ṁ acc , is a key quantity for the understanding of the physical processes governing the evolution of accretion discs around young low-mass ( M ⋆  ≲ 2.0 M ⊙ ) stars and substellar objects (YSOs). We present here the results of a study of the stellar and accretion properties of the (almost) complete sample of class II and transitional YSOs in the Lupus I, II, III and IV clouds, based on spectroscopic data acquired with the VLT/X-shooter spectrograph. Our study combines the dataset from our previous work with new observations of 55 additional objects. We have investigated 92 YSO candidates in total, 11 of which have been definitely identified with giant stars unrelated to Lupus. The stellar and accretion properties of the 81 bona fide YSOs, which represent more than 90% of the whole class II and transition disc YSO population in the aforementioned Lupus clouds, have been homogeneously and self-consistently derived, allowing for an unbiased study of accretion and its relationship with stellar parameters. The accretion luminosity, L acc , increases with the stellar luminosity, L ⋆ , with an overall slope of ~1.6, similar but with a smaller scatter than in previous studies. There is a significant lack of strong accretors below L ⋆  ≈ 0.1  L ⊙ , where L acc is always lower than 0.01  L ⋆ . We argue that the L acc  −  L ⋆ slope is not due to observational biases, but is a true property of the Lupus YSOs. The log  Ṁ acc – log  M ⋆ correlation shows a statistically significant evidence of a break, with a steeper relation for M ⋆  ≲ 0.2  M ⊙ and a flatter slope for higher masses. The bimodality of the Ṁ acc – M ⋆ relation is confirmed with four different evolutionary models used to derive the stellar mass. The bimodal behaviour of the observed relationship supports the importance of modelling self-gravity in the early evolution of the more massive discs, but other processes, such as photo-evaporation and planet formation during the YSO’s lifetime, may also lead to disc dispersal on different timescales depending on the stellar mass. The sample studied here more than doubles the number of YSOs with homogeneously and simultaneously determined L acc and luminosity, L line , of many permitted emission lines. Hence, we also refined the empirical relationships between L acc and L line on a more solid statistical basis.

Mapping water in protostellar outflows with Herschel - PACS and HIFI observations of L1448-C

Context. Water is a key probe of shocks and outflows from young stars because it is extremely sensitive to both the physical conditions associated with the interaction of supersonic outflows with the ambient medium and the chemical processes at play. Aims. Our goal is to investigate the spatial and velocity distribution of H2O along outflows, its relationship with other tracers, and its abundance variations. In particular, this study focuses on the outflow driven by the low-mass protostar L1448-C, which previous observations have shown to be one of the brightest H2O emitters among the class 0 outflows. Methods. To this end, maps of the o-H2O 1(10)-1(01) and 2(12)-1(01) transitions taken with the Herschel-HIFI and PACS instruments, respectively, are presented. For comparison, complementary maps of the CO(3-2) and SiO(8-7) transitions, obtained at the JCMT, and the H-2 S(0) and S(1) transitions, taken from the literature, were used as well. Physical conditions and H2O column densities were inferred using large velocity gradient radiative transfer calculations. Results. The water distribution appears to be clumpy, with individual peaks corresponding to shock spots along the outflow. The bulk of the 557 GHz line is confined to radial velocities in the range +/- 10-50 km s(-1), but extended emission at extreme velocities (up to v(r) similar to 80 km s(-1)) is detected and is associated with the L1448-C extreme high-velocity (EHV) jet. The H2O 1(10)-1(01)/CO(3-2) ratio shows strong variations as a function of velocity that likely reflect different and changing physical conditions in the gas that is responsible for the emissions from the two species. In the EHV jet, a low H2O/SiO abundance ratio is inferred, which could indicate molecular formation from dust-free gas directly ejected from the proto-stellar wind. The ratio between the two observed H2O lines and the comparison with H-2 indicate averaged T-kin and n(H-2) values of similar to 300-500 K and 5 x 10(6) cm(-3), respectively, while a water abundance with respect to H-2 of about 0.5-1x10(-6) along the outflow is estimated, in agreement with results found by previous studies. The fairly constant conditions found all along the outflow imply that evolutionary effects on the timescales of outflow propagation do not play a major role in the H2O chemistry. Conclusions. The results of our analysis show that the bulk of the observed H2O lines comes from post-shocked regions where the gas, after being heated to high temperatures, has already been cooled down to a few hundred K. The relatively low derived abundances, however, call for some mechanism that diminishes the H2O gas in the post-shock region. Among the possible scenarios, we favor H2O photodissociation, which requires the superposition of a low-velocity nondissociative shock with a fast dissociative shock able to produce a far-ultraviolet field of sufficient strength.