A CATALOG OF LOW-MASS STAR-FORMING CORES OBSERVED WITH SHARC-II AT 350 μm

Suresh, Akshaya; Dunham, Michael M.; Arce, Héctor G.; Evans, Neal J.; Bourke, Tyler L.; Merello, Manuel; Wu, Jingwen

doi:10.3847/0004-6256/152/2/36

Cited by 9 publications

(7 citation statements)

References 86 publications

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“…In order to estimate the increase of (accretion) luminosity, we assembled the spectral energy distribution (SED) from Cutri et al (2003) for 2MASS JHK photometry, from Dunham et al (2015) for Spitzer photometry from 3. µm and 160 µm photometry, Suresh et al (2016) for SHARC-II 350 µm, and our own 850 µm data. The observed SED (Figure 5) is deconstructed into several temperature components to evaluate what change in luminosity could reproduce the significant variability seen in the sub-mm flux.…”

Section: The Sedmentioning

confidence: 86%

The JCMT Transient Survey: Detection of Submillimeter Variability in a Class I Protostar EC 53 in Serpens Main

Yoo

Lee

Mairs

et al. 2017

ApJ

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During the protostellar phase of stellar evolution, accretion onto the star is expected to be variable, but this suspected variability has been difficult to detect because protostars are deeply embedded. In this paper, we describe a sub-mm luminosity burst of the Class I protostar EC 53 in Serpens Main, the first variable found during our dedicated JCMT/SCUBA-2 monitoring program of eight nearby star-forming regions. EC 53 remained quiescent for the first 6 months of our survey, from February to August 2016. The sub-mm emission began to brighten in September 2016, reached a peak brightness of 1.5 times the faint state, and has been decaying slowly since February 2017. The change in submm brightness is interpreted as dust heating in the envelope, generated by a luminosity increase of the protostar of a factor of ≥ 4. The 850 µm lightcurve resembles the historical K-band lightcurve, which varies by a factor of ∼ 6 with a 543 period and is interpreted as accretion variability excited by interactions between the accretion disk and a close binary system. The predictable detections of accretion variability observed at both near-infrared and sub-mm wavelengths make the system a unique test-bed, enabling us to capture the moment of the accretion burst and to study the consequences of the outburst on the protostellar disk and envelope.

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Section: The Sedmentioning

confidence: 86%

The JCMT Transient Survey: Detection of Submillimeter Variability in a Class I Protostar EC 53 in Serpens Main

Yoo

Lee

Mairs

et al. 2017

ApJ

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“…SMM4A and SMM4B are not detected by Spitzer and only marginally with Herschel where they are much fainter than a neighboring Class 0 protostar. Figure 2c shows the SED of the overall submillimeter condensation SMM4 as defined by the JCMT and derived from Spizter IRAC (3.6, 4.5, 5.8, 8.0 µm), Spizter MIPS 24 µm, Herschel PACS 70 µm observations, ALMA 1.3 mm (this work), and the literature: CSO SHARK-II 350 µm (Suresh et al 2016), JCMT SCUBA 450 µm and 850 µm (Davis et al 1999), and CARMA 3 mm (Lee et al 2014). The upper limits in the SED, which are set to be the flux densities 2.…”

Section: Spectral Energy Distributionmentioning

confidence: 88%

The Distinct Evolutionary Nature of Two Class 0 Protostars in Serpens Main SMM4

Aso

Hirano

Aikawa

et al. 2018

ApJ

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We have observed the submillimeter continuum condensation SMM4 in Serpens Main using the Atacama Large Millimeter/submillimeter Array (ALMA) during its Cycle 3 in 1.3 mm continuum, 12 CO J = 2 − 1, SO J N = 6 5 − 5 4 , and C 18 O J = 2−1 lines at angular resolutions of ∼ 0. 55 (240 au). The 1.3 mm continuum emission shows that SMM4 is spatially resolved into two protostars embedded in the same core: SMM4A showing a high brightness temperature, 18 K, with little extended structure and SMM4B showing a low brightness temperature, 2 K, with compact and extended structures. Their separation is ∼ 2100 au. Analysis of the continuum visibilities reveals a disk-like structure with a sharp edge at r ∼ 240 au in SMM4A, and a compact component with a radius of 56 au in SMM4B. The 12 CO emission traces fan-shaped and collimated outflows associated with SMM4A and SMM4B, respectively. The blue and red lobes of the SMM4B outflow have different position angles by ∼ 30 • . Their inclination and bending angles in the 3D space are estimated at i b ∼ 36 • , i r ∼ 70 • , and α ∼ 40 • , respectively. The SO emission traces shocked regions, such as cavity walls of outflows and the vicinity of SMM4B. The C 18 O emission mainly traces an infalling and rotating envelope around SMM4B. The C 18 O fractional abundance in SMM4B is ∼ 50 times smaller than that of the interstellar medium. These results suggest that SMM4A is more evolved than SMM4B. Our studies in Serpens Main demonstrate that continuum and line observations at millimeter wavelengths allow us to differentiate evolutionary phases of protostars within the Class 0 phase.

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“…Only Per-emb-39 and Per-emb-60 are marginally detected in the 1.3 mm continuum (Figure 3). Based on CSO SHARC-II (Suresh et al 2016) and JCMT SCUBA-2 (Chen et al 2016) single dish observations, Per-emb-39 and Per-emb-60 also have evidence of compact structure, while Per-emb-4 questionably does as well. However, based on these single dish observations and Herschel archival observations, no strong compact emission is evident for Per-emb-43, Per-emb-45, and Peremb-59.…”

Section: Masses Targets That May Not Be Protostarsmentioning

confidence: 99%

Mass Assembly of Stellar Systems and Their Evolution with the SMA (MASSES)—1.3 mm Subcompact Data Release

Stephens

Dunham

Myers

et al. 2018

ApJS

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We present the Mass Assembly of Stellar Systems and their Evolution with the SMA (MASSES) survey, which uses the Submillimeter Array (SMA) interferometer to map the continuum and molecular lines for all 74 known Class 0/I protostellar systems in the Perseus molecular cloud. The primary goal of the survey is to observe an unbiased sample of young protostars in a single molecular cloud so that we can characterize the evolution of protostars. This paper releases the MASSES 1.3 mm data from the subcompact configuration (∼4 or ∼1000 au resolution), which is the SMA's most compact array configuration. We release both uv visibility data and imaged data for the spectral lines CO(2-1), 13 CO(2-1), C 18 O(2-1), and N 2 D + (3-2), as well as for the 1.3 mm continuum. We identify the tracers that are detected toward each source. We also show example images of continuum and CO(2-1) outflows, analyze C 18 O(2-1) spectra, and present data from the SVS 13 star-forming region. The calculated envelope masses from the continuum show a decreasing trend with bolometric temperature (a proxy for age). Typical C 18 O(2-1) linewidths are 1.45 km s −1 , which is higher than the C 18 O linewidths detected toward Perseus filaments and cores. We find that N 2 D + (3-2) is significantly more likely to be detected toward younger protostars. We show that the protostars in SVS 13 are contained within filamentary structures as traced by C 18 O(2-1) and N 2 D + (3-2). We also present the locations of SVS 13A's high velocity (absolute line-of-sight velocities >150 km s −1 ) red and blue outflow components. Data can be downloaded from https://dataverse.harvard.edu/dataverse/MASSES.

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A CATALOG OF LOW-MASS STAR-FORMING CORES OBSERVED WITH SHARC-II AT 350 μm

Cited by 9 publications

References 86 publications

The JCMT Transient Survey: Detection of Submillimeter Variability in a Class I Protostar EC 53 in Serpens Main

The JCMT Transient Survey: Detection of Submillimeter Variability in a Class I Protostar EC 53 in Serpens Main

The Distinct Evolutionary Nature of Two Class 0 Protostars in Serpens Main SMM4

Mass Assembly of Stellar Systems and Their Evolution with the SMA (MASSES)—1.3 mm Subcompact Data Release

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