A<i>HERSCHEL</i>AND APEX CENSUS OF THE REDDEST SOURCES IN ORION: SEARCHING FOR THE YOUNGEST PROTOSTARS

Stutz, Amelia M.; Tobin, John J.; Stanke, T.; Megeath, S. Thomas; Fischer, William J.; Robitaille, Thomas; Henning, Thomas; Ali, B.; Francesco, James Di; Furlan, Elise; Hartmann, L.; Osorio, M. R. Zapatero; Wilson, Thomas L.; Allen, Lori; Krause, O.; Manoj, P.

doi:10.1088/0004-637x/767/1/36

Cited by 179 publications

(375 citation statements)

References 118 publications

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“…One of the peaks (core #11) is close (3. ′′ 5, or ∼1 500 AU) to a Class 0 protostar that has exceptionally high envelope density and mass-infall rate, discovered by Stutz et al (2013) (referred to as the PACS Bright Red Sources, PBRSs). The configuration of the two strongest peaks (cores #11 and #12) bears resemblance to the Bok Globule CB 244 in which a starless core and a young protostar co-exist within a common envelope (Stutz et al 2010).…”

Section: Structure Of the Omc-2/3 At 1 000 Au Resolutionmentioning

confidence: 99%

“…This means that building a complete view of their structure requires high resolution mapping over a large area. Coupling the gas structure with star formation also requires an accurate census of the young (proto-) stellar population of the cloud; this limits the possible targets to distances closer than ∼1 kpc where such a census can be attained (e.g., Evans et al 2009;Gutermuth et al 2011;Megeath et al 2012;Stutz et al 2013;Megeath et al 2016).…”

Section: Introductionmentioning

confidence: 99%

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Resolving the fragmentation of high line-mass filaments with ALMA: the integral shaped filament in Orion A

Kainulainen

Stutz

Stanke³

et al. 2017

A&A

114

151

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We study the fragmentation of the nearest high line-mass filament, the integral shaped filament (ISF, line-mass ∼ 400 M ⊙ pc −1 ) in the Orion A molecular cloud. We have observed a 1.6 pc long section of the ISF with the Atacama Large Millimetre/submillimeter Array (ALMA) at 3 mm continuum emission, at a resolution of ∼3 ′′ (1 200 AU). We identify from the region 43 dense cores with masses about a solar mass. 60% of the ALMA cores are protostellar and 40% are starless. The nearest neighbour separations of the cores do not show a preferred fragmentation scale; the frequency of short separations increases down to 1 200 AU. We apply a twopoint correlation analysis on the dense core separations and show that the ALMA cores are significantly grouped at separations below ∼17 000 AU and strongly grouped below ∼6 000 AU. The protostellar and starless cores are grouped differently: only the starless cores group strongly below ∼6 000 AU. In addition, the spatial distribution of the cores indicates periodic grouping of the cores into groups of ∼30 000 AU in size, separated by ∼50 000 AU. The groups coincide with dust column density peaks detected by Herschel. These results show hierarchical, two-mode fragmentation in which the maternal filament periodically fragments into groups of dense cores. Critically, our results indicate that the fragmentation models for lower line-mass filaments (∼ 16 M ⊙ pc −1 ) fail to capture the observed properties of the ISF. We also find that the protostars identified with Spitzer and Herschel in the ISF are grouped at separations below ∼17 000 AU. In contrast, young stars with disks do not show significant grouping. This suggests that the grouping of dense cores is partially retained over the protostar lifetime, but not over the lifetime of stars with disks. This is in agreement with a scenario where protostars are ejected from the maternal filament by the slingshot mechanism, a model recently proposed for the ISF by Stutz & Gould. The separation distributions of the dense cores and protostars may also provide an evolutionary tracer of filament fragmentation.

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Section: Structure Of the Omc-2/3 At 1 000 Au Resolutionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Resolving the fragmentation of high line-mass filaments with ALMA: the integral shaped filament in Orion A

Kainulainen

Stutz

Stanke³

et al. 2017

A&A

114

151

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“…For such a calculation, we first assume that objects that are mid-infrared (MIR) dark (λ < 100 µm) are starless, and cores bright at 70 µm (our PACS cores) are actively forming protostars, which has been shown as a good diagnostic for embedded protostars (Dunham et al 2008;R12;Stutz et al 2013). This differs slightly from commonly adopted criteria of the previous studies that lacked supporting Herschel data.…”

Section: Core Lifetimesmentioning

confidence: 99%

“…We also plot the upper limits in L bol for the SABOCA leaves, which lie already distinctly below the recovered core population. Cold cores have similar L bol to PACS cores in their common mass range.For comparison, we plot the luminosities and masses derived in R12 for all cores in the eleven IRDCs of the present sample, and the sample of the youngest Orion protostars (PBRs) from Stutz et al (2013). We show the empirical loci derived by Molinari et al (2008) and Saraceno et al (1996).…”

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confidence: 99%

APEX/SABOCA observations of small-scale structure of infrared-dark clouds

Ragan

Henning

Beuther

2013

A&A

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Infrared-dark clouds (IRDCs) harbor the early phases of cluster and high-mass star formation and are comprised of cold (∼20 K), dense (n > 10 4 cm −3 ) gas. The spectral energy distribution (SED) of IRDCs is dominated by the far-infrared and millimeter wavelength regime, and our initial Herschel study examined IRDCs at the peak of the SED with high angular resolution. Here we present a follow-up study using the SABOCA instrument on APEX which delivers 7.8 angular resolution at 350 µm, matching the resolution we achieved with Herschel/PACS, and allowing us to characterize substructure on ∼0.1 pc scales. Our sample of 11 nearby IRDCs are a mix of filamentary and clumpy morphologies, and the filamentary clouds show significant hierarchical structure, while the clumpy IRDCs exhibit little hierarchical structure. All IRDCs, regardless of morphology, have about 14% of their total mass in small scale core-like structures which roughly follow a trend of constant volume density over all size scales. Out of the 89 protostellar cores we identified in this sample with Herschel, we recover 40 of the brightest and re-fit their SEDs and find their properties agree fairly well with our previous estimates ( T ∼ 19 K). We detect a new population of "cold cores" which have no 70 µm counterpart, but are 100 and 160 µm-bright, with colder temperatures ( T ∼ 16 K). This latter population, along with SABOCA-only detections, are predominantly low-mass objects, but their evolutionary diagnostics are consistent with the earliest starless or prestellar phase of cores in IRDCs.Key words. catalogs -stars: formation -ISM: structure -submillimeter: ISM Background and motivationDespite the importance of high-mass stars to the energy budget of galaxies, their formation remains a major open question in astronomy (Zinnecker & Yorke 2007). A major hindrance to progress is the inherent difficulty in obtaining well-defined initial conditions observationally. Because high-mass stars are rare, they are on average at large distances, thus angular resolution is of paramount importance. With the advent of Spitzer Space Telescope and Herschel Space Observatory (Pilbratt et al. 2010), coupled with extensive ground-based survey efforts, we now can approach this observational task statistically.Ever since their discovery in absorption in mid-infrared Galactic plane surveys, ISO data (Perault et al. 1996) and MSX observations (Egan et al. 1998), infrared-dark clouds (IRDCs) have been subject to intense study because they are the cold (T < 20 K), dense (n > 10 4 cm −3 ) environments believed to be required for the formation of high-mass stars and clusters (cf. Rathborne et al. 2006;Ragan et al. 2009;Battersby et al. 2010). They are located throughout the Galactic plane, concentrated within the spiral arms (Jackson et al. 2008). The formation of IRDCs, their kinematic structure and population of Based on observations carried out with the Atacama Pathfinder Experiment (APEX). APEX is a collaboration between Max Planck Institut für Radioastronomie (MPIf...

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“…The circumstellar gas and dust (disk or envelope) produces an excess of infrared (IR) emission that can be used as a diagnostic tool (e.g., Allen et al 2004;Hartmann et al 2005). Infrared color-color diagrams have been widely used to distinguish between different types of YSOs in different star-forming regions (see Gutermuth et al 2009;Luhman et al 2010;Rebull et al 2011;Koenig et al 2012;Megeath et al 2012;Spezzi et al 2013;Stutz et al 2013;Broekhoven-Fiene et al 2014;Esplin et al 2014, as recent examples). The accretion of this surrounding material onto the surface of the star produces intense ultraviolet (UV) line and continuum emission also observed as an excess over the predicted photospheric emission.…”

Section: Introductionmentioning

confidence: 99%

Young stellar object candidates toward the Orion region selected from GALEX

Sánchez

Castro

López-Martínez

et al. 2014

A&A

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We analyze 359 ultraviolet tiles from the All Sky Imaging Survey of the space mission GALEX covering roughly 400 square degrees toward the Orion star-forming region. There are a total of 1 555 174 ultraviolet sources that were cross-matched with other catalogs (2MASS, UCAC4, SDSS, DENIS, CMC15, and WISE) to produce a list of 290 717 reliable sources with a wide range of photometric information. Using different color selection criteria, we identify 111 young stellar object candidates showing both ultraviolet and infrared excesses, of which 81 are new identifications. We discuss the spatial distribution, the spectral energy distributions, and other physical properties of these stars. Their properties are, in general, compatible with those expected for T Tauri stars. This population of TTS candidates is widely dispersed around the Orion molecular cloud.

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

Cited by 179 publications

References 118 publications

Resolving the fragmentation of high line-mass filaments with ALMA: the integral shaped filament in Orion A

Resolving the fragmentation of high line-mass filaments with ALMA: the integral shaped filament in Orion A

APEX/SABOCA observations of small-scale structure of infrared-dark clouds

Young stellar object candidates toward the Orion region selected from GALEX

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