<i>Spitzer</i>and HHT Observations of Bok Globule B335: Isolated Star Formation Efficiency and Cloud Structure

Stutz, Amelia M.; Rubin, M.; Werner, M. W.; Rieke, G. H.; Bieging, John H.; Keene, J.; Kang, Miju; Shirley, Yancy L.; Su, K. Y. L.; Velusamy, T.; Wilner, David J.

doi:10.1086/591789

Cited by 56 publications

(53 citation statements)

References 67 publications

(121 reference statements)

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“…Regardless of evolutionary state, the outflow cavities enable near-to mid-infrared light from the protostar and disk to escape and scatter off dust grains in the cavity or on the cavity walls. This phenomenon has been well known for Class I sources (Kenyon et al 1993;Padgett et al 1999), but Class 0 protostars were only well detected in the midinfrared with Spitzer (Noriega-Crespo et al 2004;Jørgensen et al 2007;Stutz et al 2008). The scattered light from Class 0 protostars is often brightest at wavelengths ∼3.6 μm or 4.5 μm due to the dense envelope obscuration at shorter wavelengths (e.g., Whitney et al 2003b;Tobin et al 2007).…”

Section: Introductionmentioning

confidence: 85%

“…In Figure 6, we show the MIPS 24 μm, PACS 70 μm, and PACS 160 μm colors of the new Herschel sources compared to (Stutz et al 2008;Launhardt et al 2013), CB68 (Launhardt et al 2013), and CB244 Launhardt et al 2013). Furthermore, we also show the colors of various VeLLOs: L673-7 (Dunham et al 2008), IRAM04191 (Dunham et al 2006), and CB130 (Launhardt et al 2013).…”

Section: Herschel Protostar Candidatesmentioning

confidence: 99%

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AHERSCHELAND APEX CENSUS OF THE REDDEST SOURCES IN ORION: SEARCHING FOR THE YOUNGEST PROTOSTARS

Stutz

Tobin

Stanke³

et al. 2013

ApJ

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179

357

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We perform a census of the reddest, and potentially youngest, protostars in the Orion molecular clouds using data obtained with the PACS instrument on board the Herschel Space Observatory and the LABOCA and SABOCA instruments on APEX as part of the Herschel Orion Protostar Survey (HOPS). A total of 55 new protostar candidates are detected at 70 μm and 160 μm that are either too faint (m 24 > 7 mag) to be reliably classified as protostars or undetected in the Spitzer/MIPS 24 μm band. We find that the 11 reddest protostar candidates with log λF λ 70/λF λ 24 > 1.65 are free of contamination and can thus be reliably explained as protostars. The remaining 44 sources have less extreme 70/24 colors, fainter 70 μm fluxes, and higher levels of contamination. Taking the previously known sample of Spitzer protostars and the new sample together, we find 18 sources that have log λF λ 70/λF λ 24 > 1.65; we name these sources "PACS Bright Red sources," or PBRs. Our analysis reveals that the PBR sample is composed of Class 0 like sources characterized by very red spectral energy distributions (SEDs; T bol < 45 K) and large values of sub-millimeter fluxes (L smm /L bol > 0.6%). Modified blackbody fits to the SEDs provide lower limits to the envelope masses of 0.2-2 M and luminosities of 0.7-10 L . Based on these properties, and a comparison of the SEDs with radiative transfer models of protostars, we conclude that the PBRs are most likely extreme Class 0 objects distinguished by higher than typical envelope densities and hence, high mass infall rates.

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Section: Introductionmentioning

confidence: 85%

Section: Herschel Protostar Candidatesmentioning

confidence: 99%

AHERSCHELAND APEX CENSUS OF THE REDDEST SOURCES IN ORION: SEARCHING FOR THE YOUNGEST PROTOSTARS

Stutz

Tobin

Stanke³

et al. 2013

ApJ

Self Cite

179

357

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“…This isolated source at the distance of 150 pc (Stutz et al 2008) harbors several HerbigHaro objects associated with a bipolar outflow (see e.g. Gålfalk & Olofsson 2007).…”

Section: B335mentioning

confidence: 99%

Odin observations of water in molecular outflows and shocks

Bjerkeli¹,

Liseau²,

Olberg

et al. 2009

A&A

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Aims. We investigate the ortho-water abundance in outflows and shocks in order to improve our knowledge of shock chemistry and of the physics behind molecular outflows. Methods. We used the Odin space observatory to observe the H 2 O(1 10 −1 01 ) line. We obtain strip maps and single pointings of 13 outflows and two supernova remnants where we report detections for eight sources. We used RADEX to compute the beam averaged abundances of o-H 2 O relative to H 2 . In the case of non-detection, we derive upper limits on the abundance. Results. Observations of CO emission from the literature show that the volume density of H 2 can vary to a large extent, a parameter that puts severe uncertainties on the derived abundances. Our analysis shows a wide range of abundances reflecting the degree to which shock chemistry affects the formation and destruction of water. We also compare our results with recent results from the SWAS team. Conclusions. Elevated abundances of ortho-water are found in several sources. The abundance reaches values as high as what would be expected from a theoretical C-type shock where all oxygen, not in the form of CO, is converted to water. However, the high abundances we derive could also be due to the low densities (derived from CO observations) that we assume. The water emission may in reality stem from high density regions much smaller than the Odin beam. We do not find any relationship between the abundance and the mass loss rate. On the other hand, there is a relation between the derived water abundance and the observed maximum outflow velocity.

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“…The maps show a dark patch against the nebulous far-IR emission that closely resembles the dark patch seen at visible wavelengths. The MSX, ISO, and Spitzer space telescopes have detected clouds in absorption at mid-IR (5-30 μm) wavelengths against the diffuse IR background of the Galaxy (e.g., Bacmann et al 2000;Stutz et al 2008;Tobin et al 2010;Stutz et al 2009a), in a few cases even at 70 μm (Stutz et al 2009b). However, the detection of the NGC 1999 globule by PACS would be the first detection of a dark globule in absorption at 160 μm.…”

Section: Introductionmentioning

confidence: 99%

Hier ist wahrhaftig ein Loch im Himmel

Stanke¹,

Stutz

Tobin

et al. 2010

A&A

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The NGC 1999 reflection nebula features a dark patch with a size of ∼10 000 AU, which has been interpreted as a small, dense foreground globule and possible site of imminent star formation. We present Herschel PACS far-infrared 70 and 160 μm maps, which reveal a flux deficit at the location of the globule. We estimate the globule mass needed to produce such an absorption feature to be a few tenths to a few M . Inspired by this Herschel observation, we obtained APEX LABOCA and SABOCA submillimeter continuum maps, and Magellan PANIC near-infrared images of the region. We do not detect a submillimer source at the location of the Herschel flux decrement; furthermore our observations place an upper limit on the mass of the globule of ∼2.4 × 10 −2 M . Indeed, the submillimeter maps appear to show a flux depression as well. Furthermore, the near-infrared images detect faint background stars that are less affected by extinction inside the dark patch than in its surroundings. We suggest that the dark patch is in fact a hole or cavity in the material producing the NGC 1999 reflection nebula, excavated by protostellar jets from the V 380 Ori multiple system.

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Spitzerand HHT Observations of Bok Globule B335: Isolated Star Formation Efficiency and Cloud Structure

Cited by 56 publications

References 67 publications

AHERSCHELAND APEX CENSUS OF THE REDDEST SOURCES IN ORION: SEARCHING FOR THE YOUNGEST PROTOSTARS

AHERSCHELAND APEX CENSUS OF THE REDDEST SOURCES IN ORION: SEARCHING FOR THE YOUNGEST PROTOSTARS

Odin observations of water in molecular outflows and shocks

Hier ist wahrhaftig ein Loch im Himmel

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