The Vla Nascent Disk and Multiplicity Survey of Perseus Protostars (Vandam). Ii. Multiplicity of Protostars in the Perseus Molecular Cloud

Tobin, John J.; Looney, Leslie W.; Li, Zhi-Yun; Chandler, Claire J.; Dunham, Michael M.; Segura-Cox, Dominique; Sadavoy, Sarah; Melis, Carl; Harris, Robert J.; Kratter, Kaitlin M.; Pérez, Laura

doi:10.3847/0004-637x/818/1/73

Cited by 265 publications

(530 citation statements)

References 139 publications

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“…companion properties to solar-type primaries may differ in young star-forming environments (Duchêne et al 2007;Connelley et al 2008b;Kraus et al 2011;Tobin et al 2016), in dense open clusters (Patience et al 2002;Köhler et al 2006;Geller & Mathieu 2012;King et al 2012), or at extremely low metallicities (Abt 2008;Gao et al 2014;Hettinger et al 2015). In Section 10, we compare the corrected solar-type binary statistics of the field MS population to those of younger MS and pre-MS populations in open clusters and stellar associations.…”

Section: Sample Selectionmentioning

confidence: 99%

Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars

Moe

Stefano

2017

ApJS

1,094

1,200

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We compile observations of early-type binaries identified via spectroscopy, eclipses, long-baseline interferometry, adaptive optics, common proper motion, etc. Each observational technique is sensitive to companions across a narrow parameter space of orbital periods P and mass ratios q=M comp /M 1 . After combining the samples from the various surveys and correcting for their respective selection effects, we find that the properties of companions to O-type and B-type main-sequence (MS) stars differ among three regimes. First, at short orbital periods P20days (separations a0.4 au), the binaries have small eccentricities e0.4, favor modest mass ratios á ñ » q 0.5, and exhibit a small excess of twins q>0.95. Second, the companion frequency peaks at intermediate periods log P (days)≈3.5 (a ≈ 10 au), where the binaries have mass ratios weighted toward small values q≈0.2-0.3 and follow a Maxwellian "thermal" eccentricity distribution. Finally, companions with long orbital periods log P (days)≈5.5-7.5 (a ≈ 200-5000 au) are outer tertiary components in hierarchical triples and have a mass ratio distribution across q≈0.1-1.0 that is nearly consistent with random pairings drawn from the initial mass function. We discuss these companion distributions and properties in the context of binary-star formation and evolution. We also reanalyze the binary statistics of solar-type MS primaries, taking into account that 30% ±10% of single-lined spectroscopic binaries likely contain white dwarf companions instead of low-mass stellar secondaries. The mean frequency of stellar companions with q>0.1 and log P (days)<8.0 per primary increases from 0.50±0.04 for solar-type MS primaries to 2.1±0.3 for O-type MS primaries. We fit joint probability density functions ¹ ( ) ( ) ( ) ( ) ( ) f M q P e f M f q f P f e , , , 1 1 to the corrected distributions, which can be incorporated into binary population synthesis studies.

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Section: Sample Selectionmentioning

confidence: 99%

Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars

Moe

Stefano

2017

ApJS

1,094

1,200

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“…The continuum map of NGC1333-IRAS2A reveals the main protostar IRAS2-A1, plus two weaker peaks, IRAS2-A2 and IRAS2-A3 (see Codella et al 2014). The nature of A2 and A3 is still debated, being possibly dust fragments associated with the molecular cloud and swept up by the outflows driven by the nearby IRAS2-A1 protostar (see Codella et al 2014;Tobin et al 2016). For the purpose of the analysis presented in this paper, we have considered these as genuine protostars, except where explicitly mentioned otherwise.…”

Section: The Samplementioning

confidence: 99%

“…• southwest of NGC1333, while L1448-C is located at the center of the L1148 complex (see Looney et al 2000;Tobin et al 2016, and references therein).…”

Section: The Samplementioning

confidence: 99%

Glycolaldehyde in Perseus young solar analogs

Simone

Codella

Testi

et al. 2017

A&A

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Context. The earliest evolutionary stages of low-mass protostars are characterised by the so-called hot-corino stage, when the newly born star heats the surrounding material and enrich the gas chemically. Studying this evolutionary phase of solar protostars may help understand the evolution of prebiotic complex molecules in the development of planetary systems. Aims. In this paper we focus on the occurrence of glycolaldehyde (HCOCH 2 OH) in young solar analogs by performing the first homogeneous and unbiased study of this molecule in the Class 0 protostars of the nearby Perseus star forming region. Methods. We obtained sub-arcsec angular resolution maps at 1.3mm and 1.4mm of glycolaldehyde emission lines using the IRAM Plateau de Bure (PdB) interferometer in the framework of the CALYPSO IRAM large program. Results. Glycolaldehyde has been detected towards 3 Class 0 and 1 Class I protostars out of the 13 continuum sources targeted in Perseus: NGC1333-IRAS2A1, NGC1333-IRAS4A2, NGC1333-IRAS4B1, and SVS13-A. The NGC1333 star forming region looks particularly glycolaldehyde rich, with a rate of occurrence up to 60%. The glycolaldehyde spatial distribution overlaps with the continuum one, tracing the inner 100 au around the protostar. A large number of lines (up to 18), with upper-level energies E u from 37 K up to 375 K has been detected. We derived column densities ≥ 10 15 cm −2 and rotational temperatures T rot between 115 K and 236 K, imaging for the first time hot-corinos around NGC1333-IRAS4B1 and SVS13-A. Conclusions. In multiple systems glycolaldehyde emission is detected only in one component. The case of the SVS13-A+B and IRAS4-A1+A2 systems support that the detection of glycolaldehyde (at least in the present Perseus sample) indicates older protostars (i.e. SVS13-A and IRAS4-A2), evolved enough to develop the hot-corino region (i.e. 100 K in the inner 100 au). However, only two systems do not allow us to firmly conclude whether the primary factor leading to the detection of glycolaldehyde emission is the environments hosting the protostars, evolution (e.g. low value of L submm /L int ), or accretion luminosity (high L int ).

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“…With the results from the VANDAM survey of Tobin et al (2016), we have access to the full binary statistics of the protostars in Perseus down to spatial scales of ∼15 AU. Of the 24 MASSES objects studied in this paper, 16 (67 %) are part of a multiple system with projected separations ranging from 0.08 to 16 (19 AU to 3760 AU).…”

Section: Link To Multiple Systemsmentioning

confidence: 99%

Protostellar accretion traced with chemistry

Frimann

Jørgensen

Dunham

et al. 2017

A&A

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Context. Understanding how accretion proceeds is a key question of star formation, with important implications for both the physical and chemical evolution of young stellar objects. In particular, very little is known about the accretion variability in the earliest stages of star formation. Aims. To characterise protostellar accretion histories towards individual sources by utilising sublimation and freeze-out chemistry of CO. Methods. A sample of 24 embedded protostars are observed with the Submillimeter Array (SMA) in context of the large program "Mass Assembly of Stellar Systems and their Evolution with the SMA" (MASSES). The size of the C 18 O emitting region, where CO has sublimated into the gas-phase, is measured towards each source and compared to the expected size of the region given the current luminosity. The SMA observations also include 1.3 mm continuum data, which are used to investigate whether a link can be established between accretion bursts and massive circumstellar disks. Results. Depending on the adopted sublimation temperature of the CO ice, between 20 % and 50 % of the sources in the sample show extended C 18 O emission indicating that the gas was warm enough in the past that CO sublimated and is currently in the process of refreezing; something which we attribute to a recent accretion burst. Given the fraction of sources with extended C 18 O emission, we estimate an average interval between bursts of 20 000 yr-50 000 yr, which is consistent with previous estimates. No clear link can be established between the presence of circumstellar disks and accretion bursts, however the three closest known binaries in the sample (projected separations <20 AU) all show evidence of a past accretion burst, indicating that close binary interactions may also play a role in inducing accretion variability.

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The Vla Nascent Disk and Multiplicity Survey of Perseus Protostars (Vandam). Ii. Multiplicity of Protostars in the Perseus Molecular Cloud

Cited by 265 publications

References 139 publications

Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars

Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars

Glycolaldehyde in Perseus young solar analogs

Protostellar accretion traced with chemistry

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