A Spectroscopic Study of Young Stellar Objects in the Serpens Cloud Core and NGC 1333

Winston, E.; Megeath, S. Thomas; Wolk, S. J.; Hernández, Jesús; Gutermuth, R. A.; Muzerolle, James; Hora, J. L.; Covey, Kevin R.; Allen, Lori; Spitzbart, B.; Peterson, Dawn E.; Myers, Philip C.; Fazio, G. G.

doi:10.1088/0004-6256/137/6/4777

Cited by 64 publications

(150 citation statements)

References 70 publications

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“…The negative features are shown by dashed lines. low-and intermediate PMS stars, and indeed, Luhman (1999) and Winston et al (2009) find that PMS spectra have a surface gravity midway between giant and dwarf spectra. If the stars were giants, dust veiling could make the K-band CO lines weaker.…”

Section: Sinfoni Stellar Spectral Type Classificationmentioning

confidence: 88%

Different evolutionary stages in the massive star-forming region S255 complex

Wang

Beuther

Bik

et al. 2011

A&A

109

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Aims. Massive stars form in clusters, and they are often found in different evolutionary stages located close to each other. To understand evolutionary and environmental effects during the formation of high-mass stars, we observed three regions of massive star formation at different evolutionary stages, and all are found that in the same natal molecular cloud. Methods. The three regions, S255IR, S255N, and S255S, were observed at 1.3 mm with the submillimeter array (SMA), and followup short spacing information was obtained with the IRAM 30 m telescope. Near infrared (NIR) H + K-band spectra and continuum observations were taken for S255IR with VLT-SINFONI to study the different stellar populations in this region.Results. This combination of millimeter (mm) and near infrared data allow us to characterize different stellar populations within the young forming cluster in detail. While we find multiple mm continuum sources toward all regions, their outflow, disk, and chemical properties vary considerably. The most evolved source S255IR exhibits a collimated bipolar outflow visible in CO and H 2 emission, and the outflows from the youngest region S255S are still small and fairly confined in the regions of the mm continuum peaks. Also the chemistry toward S255IR is the most evolved, exhibiting strong emission from complex molecules, while much fewer molecular lines are detected in S255N, and in S255S we detect only CO isotopologues and SO lines. Also, rotational structures are found toward S255N and S255IR. Furthermore, a comparison of the NIR SINFONI and mm data from S255IR clearly reveal two different (proto) stellar populations with an estimated age difference of approximately 1 Myr. Conclusions. A multiwavelength spectroscopy and mapping study reveals different evolutionary phases of the star formation regions. We propose the triggered outside-in collapse star formation scenario for the bigger picture and the fragmentation scenario for S255IR.

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Section: Sinfoni Stellar Spectral Type Classificationmentioning

confidence: 88%

Different evolutionary stages in the massive star-forming region S255 complex

Wang

Beuther

Bik

et al. 2011

A&A

109

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“…The extinction is computed for each candidate using the extinction vector and regressing the objects back towards the 3 Myr PMS isochrone (Chabrier et al 2000), i.e. the typical age of the Serpens cloud core population (Winston et al 2009;Oliveira et al 2009). The extinction values derived through this method (A 3 My V ) are reported in Table 4.…”

Section: Reddening and Spectral Type Estimatesmentioning

confidence: 99%

“…The Serpens Core region is an example of a very young, deeply embedded (A V ≈ 40 mag) cluster, containing a high percentage of protostars (Davis et al 1999;Testi et al 2000;Kaas et al 2004;Eiroa et al 2006;Harvey et al 2007;Winston et al 2007). With an age between 2 and ∼6 Myr (Winston et al 2009;Oliveira et al 2009) and a distance estimated between 260 ± 37 pc (Straižys et al 2003) and 415 ± 5 pc (Dzib et al 2010), the Serpens cloud core is one of the nearest regions of clustered star formation to the Sun. Therefore, it is an excellent candidate for study as it is close enough to both resolve the individual members and detect the lowest mass members to below the hydrogen-burning limit.…”

Section: Introductionmentioning

confidence: 99%

“…Therefore, it is an excellent candidate for study as it is close enough to both resolve the individual members and detect the lowest mass members to below the hydrogen-burning limit. Throughout this paper, we assume a typical age of 3 Myr (Winston et al 2009) for the Serpens Core cluster and the minimum distance of 260 ± 37 pc (Straižys et al 2003) 1 . The region is also particularly interesting for BD studies because only a few dedicated searches have been reported in the literature.…”

Section: Introductionmentioning

confidence: 99%

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Searching for planetary-mass T-dwarfs in the core of Serpens

Spezzi

Oliveira

Moraux

et al. 2012

A&A

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Context. The knowledge of the present-day mass function of young clusters and the mass of their coolest substellar members is essential to clarify the brown dwarf formation mechanism, which still remains a matter of debate. Aims. We searched for isolated planetary-mass T-dwarfs in the ∼3 Myr old Serpens Core cluster. Methods. We performed a deep imaging survey of the central part of this cluster using the WIRCam camera at the CFHT. Observations were performed through the narrow-band CH 4 off and CH 4 on filters, to identify young T-dwarfs from their 1.6 μm methane absorption bands, and the broad-band JHK S filters, to better characterize the selected candidates. We complemented our WIRCam photometry with optical imaging data from MegaCam at CFHT and Suprime-Cam at the Subaru telescope and mid-infrared flux measurements from the Spitzer "core to disk" (c2d) Legacy Survey. Results. We report four faint T-dwarf candidates in the direction of the Serpens Core with CH 4 on−CH 4 off above 0.2 mag, estimated visual extinction in the range 1−9 mag and spectral type in the range T1−T5 based on their dereddened CH 4 on−CH 4 off colors. Comparisons with T-dwarf spectral models and optical to mid-infrared color-color and color-magnitude diagrams, indicate that two of our candidates (ID 1 and 2) are background contaminants (most likely heavily reddened low-redshift quasars). The properties of the other two candidates (ID 3 and 4) are consistent with them being young members of the Serpens Core cluster, although our analysis can not be considered conclusive. In particular, ID 3 may also be a foreground T-dwarf. It is detected by the Spitzer c2d survey but only flux upper limits are available above 5.8 μm and, hence, we can not assess the presence of a possible disk around this object. However, it presents some similarities with other young T-dwarf candidates (S Ori 70 in the σ Orionis cluster and CFHT_J0344+3206 in the direction of IC 348). If ID 3 and 4 belong to Serpens, they would have a mass of a few Jupiter masses and would be amongst the youngest, lowest mass objects detected in a star-forming region so far.

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“…Our classification of these sources follows the prescriptions of Winston et al (2009) and Bik et al (2010) for late-type stars. This comparative method uses primarily the MgI, NaI, and CaI atomic lines as diagnostics for the temperature and the CO first overtone absorption bands as luminosity indicator.…”

Section: Spectral Classificationmentioning

confidence: 99%

Near-infrared spectroscopy in NGC 7538

Puga¹,

Marín-Franch

Najarro³

et al. 2010

A&A

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Aims. The characterisation of the stellar population in young high-mass star-forming regions allows fundamental cluster properties like distance and age to be constrained. These are essential when using high-mass clusters as probes for conducting Galactic studies. Methods. NGC 7538 is a star-forming region with an embedded stellar population unearthed only in the near-infrared (NIR). We present the first near-infrared spectro-photometric study of the candidate high-mass stellar content in NGC 7538. We obtained H and K spectra of 21 sources with both the multi-object and long-slit modes of LIRIS at the WHT, and complement these data with subarcsecond JHK s photometry of the region using the imaging mode of the same instrument. Results. We find a wide variety of objects within the studied stellar population of NGC 7538. Our results discriminate between a stellar population associated to the H ii region, but not contained within its extent, and several pockets of more recent star formation.We report the detection of CO bandhead emission toward several sources, as well as other features indicative of a young stellar nature. We infer a spectro-photometric distance of 2.7 ± 0.5 kpc, an age spread in the range 0.5−2.2 Myr and a total mass ∼1.7 × 10 3 M for the older population.

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A Spectroscopic Study of Young Stellar Objects in the Serpens Cloud Core and NGC 1333

Cited by 64 publications

References 70 publications

Different evolutionary stages in the massive star-forming region S255 complex

Different evolutionary stages in the massive star-forming region S255 complex

Searching for planetary-mass T-dwarfs in the core of Serpens

Near-infrared spectroscopy in NGC 7538

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