A PANCHROMATIC VIEW OF NGC 602: TIME-RESOLVED STAR FORMATION WITH THE<i>HUBBLE</i>AND<i>SPITZER</i>SPACE TELESCOPES

Carlson, L. R.; Sewiło, M.; Meixner, Margaret; Romita, Krista; Whitney, B. A.; Hora, J. L.; Cignoni, M.; Sabbi, E.; Nota, A.; Sirianni, M.; Smith, L. J.; Babler, B.; Bracker, S.; Gallagher, John S.; Meade, M. R.; Misselt, K. A.; Pasquali, A.; Shiao, Bernie

doi:10.1088/0004-637x/730/2/78

Cited by 28 publications

(75 citation statements)

References 55 publications

(85 reference statements)

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“…The YSO model set does not include multiple sources. However, we showed in Carlson et al (2011) that the SED fitter can be used in the identification of YSOs even when they are members of protoclusters. This is in part because we expect one or two sources to dominate the luminosity of a protocluster: L YSO ∝ M each of these factors might contribute to the overall error budget for SED fitting is difficult.…”

Section: Yso Candidate Selection and Classificationmentioning

confidence: 97%

“…For fitting, we require sources meeting at least 1α criterion to have at least 4 bands of photometry defining the SED and consider a relatively large χ 2 min /pt well-fit (i.e. reduced χ 2 ; see Carlson et al 2011, for a detailed explanation). We consider sources with at least 1α selection criterion and falling within either an α or β selection region in all five CMDs to be the most reliable.…”

Section: Yso Candidate Selection and Classificationmentioning

confidence: 99%

“…The conversion from IRSF to 2MASS magnitudes introduces an additional error, but this is estimated included in the conversion as given by Kato et al (2007). Studies such as Carlson et al (2011) and Chen et al (2009) have shown that the large majority (∼70% or more) of IRAC YSO candidates at these distances are in fact (IR) dominant members of (optical) protoclusters. The YSO model set does not include multiple sources.…”

Section: Yso Candidate Selection and Classificationmentioning

confidence: 99%

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Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

Carlson

Sewiło

Meixner

et al. 2012

A&A

110

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We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine Hii regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, AJ, 132, 2268, combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997, AJ, 114, 1002 and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, PASJ, 59, 615). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007, ApJS, 169, 328) and estimate mass functions and SFRs for each region.

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Section: Yso Candidate Selection and Classificationmentioning

confidence: 97%

Section: Yso Candidate Selection and Classificationmentioning

confidence: 99%

Section: Yso Candidate Selection and Classificationmentioning

confidence: 99%

See 1 more Smart Citation

Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

Carlson

Sewiło

Meixner

et al. 2012

A&A

110

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“…This discovery showed that these MYSOs are not isolated, at least not as far as their immediate environments are concerned. The observational contradiction between high-and low-resolution imaging about the isolation of high-mass stellar sources in the Magellanic Clouds is an issue that is already discussed in the literature (e.g., Gouliermis et al 2007;Carlson et al 2011). Including our dataset, every MYSO resolved with HST is found to be surrounded by lower-mass red sources.…”

Section: Estimates Of Cluster Massesmentioning

confidence: 99%

STELLAR CLUSTERINGS AROUND “ISOLATED” MASSIVE YSOs IN THE LMC

Stephens

Gouliermis

Looney

et al. 2017

ApJ

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Observations suggest that there is a significant fraction of O-stars in the field of the Milky Way that appear to have formed in isolation or in low mass clusters (<100 M ). The existence of these high-mass stars that apparently formed in the field challenges the generally accepted paradigm, which requires star formation to occur in clustered environments. In order to understand the physical conditions for the formation of these stars, it is necessary to observe isolated high-mass stars while they are still forming. With the Hubble Space Telescope, we observe the seven most isolated massive (>8 M ) young stellar objects (MYSOs) in the Large Magellanic Cloud (LMC). The observations show that while these MYSOs are remote from other MYSOs, OB associations, and even from known giant molecular clouds, they are actually not isolated at all. Imaging reveals ∼100 to several hundred pre-main-sequence (PMS) stars in the vicinity of each MYSO. These previously undetected PMS stars form prominent compact clusters around the MYSOs, and in most cases they are also distributed sparsely across the observed regions. Contrary to what previous high-mass field star studies show, these observations suggest that high-mass stars may not be able to form in clusters with masses less than 100 M . If these MYSOs are indeed the best candidates for isolated high-mass star formation, then the lack of isolation is at odds with random sampling of the IMF. Moreover, while isolated MYSOs may not exist, we find evidence that isolated clusters containing O-stars can exist, which in itself is rare.

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“…We employed the three-dimensional radiative transfer code HOCHUNK3D for protostars, which was developed by Whitney et al (2013) based on the two-dimensional version (Whitney et al 2003a(Whitney et al , 2003b(Whitney et al , 2004) that has been widely used in previous infrared surveys of protostars (e.g., Young et al 2005;Haisch et al 2006;Bolatto et al 2007;Carlson et al 2007Carlson et al , 2011Chapman et al 2007;Harvey et al 2007;Hatchell et al 2007;Simon et al 2007;Tobin et al 2007;Merín et al 2008;Poulton et al 2008;Seale & Looney 2008;Whitney et al 2008;Enoch et al 2009;Forbrich et al 2010;Gramajo et al 2010;Samal et al 2012;Stutz et al 2013). While HOCHUNK3D is equipped to deal with spiral and warp structures and gaps in the disk, our current study is focused on the two-dimensional structures of protostellar disks and envelopes.…”

Section: Radiative Transfer Modelsmentioning

confidence: 99%

The Power of SOFIA/FORCAST in Estimating Internal Luminosities of Low-mass Class 0/I Protostars

Huard

Terebey

2017

ApJ

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With the Stratospheric Observatory for Infrared Astronomy (SOFIA) routinely operating science flights, we demonstrate that observations with the Faint Object infraRed CAmera for the SOFIA Telescope (FORCAST) can provide reliable estimates of the internal luminosities, L int , of protostars. We have developed a technique to estimate L int using a pair of FORCAST filters: one "short-wavelength" filter centered within 19.7-25.3μm, and one "long-wavelength" filter within 31.5-37.1μm. These L int estimates are reliable to within 30%-40% for 67% of protostars and to within a factor of 2.3-2.6 for 99% of protostars. The filter pair comprised of F 25.3 μm and F 37.1 μm achieves the best sensitivity and most constrained results. We evaluate several assumptions that could lead to systematic uncertainties. The OH5 dust opacity matches observational constraints for protostellar environments best, although not perfectly; we find that any improved dust model will have a small impact of 5%-10% on the L int estimates. For protostellar envelopes, the TSC84 model yields masses that are twice those of the Ulrich model, but we conclude that this mass difference does not significantly impact results at the mid-infrared wavelengths probed by FORCAST. Thus, FORCAST is a powerful instrument for luminosity studies targeting newly discovered protostars or suspected protostars lacking detections longward of 24μm. Furthermore, with its dynamic range and greater angular resolution, FORCAST may be used to characterize protostars that were either saturated or merged with other sources in previous surveys using the Spitzer Space Telescope or the Herschel Space Observatory.

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A PANCHROMATIC VIEW OF NGC 602: TIME-RESOLVED STAR FORMATION WITH THEHUBBLEANDSPITZERSPACE TELESCOPES

Cited by 28 publications

References 55 publications

Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

Identifying young stellar objects in nine Large Magellanic Cloud star-forming regions

STELLAR CLUSTERINGS AROUND “ISOLATED” MASSIVE YSOs IN THE LMC

The Power of SOFIA/FORCAST in Estimating Internal Luminosities of Low-mass Class 0/I Protostars

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