The Gould’s Belt Distances Survey (Gobelins). Iii. The Distance to the Serpens/Aquila Molecular Complex

Ortiz-León, Gisela N.; Dzib, Sergio A.; Kounkel, Marina; Loinard, Laurent; Mioduszewski, Amy J.; Rodrı́guez, Luis F.; Torres, Rosa M.; Pech, Gerardo; Rivera, Juana L.; Hartmann, L.; Boden, Andrew F.; Evans, Neal J.; Briceño, César; Tobin, John J.; Galli, P. A. B.

doi:10.3847/1538-4357/834/2/143

Cited by 130 publications

(108 citation statements)

References 50 publications

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“…The distance adopted in this work is also used in Oliveira et al (2013) and is consistent with Chandra observations of the Serpens core by Winston et al (2010). A more recent distance estimate using VLBI in the form of the GOBELINS survey is 436 ± 9 pc (Ortiz-León et al 2017). As this is only ∼5% higher than the previous values, and consistent within the 1σ errorbars, we decide to use the original distance value for consistency with Oliveira et al (2013).…”

Section: Sample Selectionmentioning

confidence: 80%

An SMA Continuum Survey of Circumstellar Disks in the Serpens Star-forming Region

Law¹,

Ricci²,

Andrews³

et al. 2017

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We present observations with the Submillimeter Array of the continuum emission at λ = 1.3 mm from 62 young stars surrounded by a protoplanetary disk in the Serpens star-forming region. The typical angular resolution for the survey in terms of beam size is 3.5 × 2.5 with a median rms noise level of 1.6 mJy beam −1 . These data are used to infer the dust content in disks around low-mass stars (0.1-2.5 M ) at a median stellar age of 1-3 Myr. Thirteen sources were detected in the 1.3 mm dust continuum with inferred dust masses of ≈10-260 M ⊕ and an upper limit to the median dust mass of 5.1 +6.1 −4.3 M ⊕ , derived using survival analysis. Comparing the protoplanetary disk population in Serpens to those of other nearby star-forming regions, we find that the populations of dust disks in Serpens and Taurus, which have a similar age, are statistically indistinguishable. This is potentially surprising since Serpens has a stellar surface density two orders of magnitude in excess of Taurus. Hence, we find no evidence that dust disks in Serpens have been dispersed as a result of more frequent and/or stronger tidal interactions due its elevated stellar density. We also report that the fraction of Serpens disks with M dust ≥ 10 M ⊕ is less than 20%, which supports the notion that the formation of giant planets is likely inherently rare or has substantially progressed by a few Myrs.

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Section: Sample Selectionmentioning

confidence: 80%

An SMA Continuum Survey of Circumstellar Disks in the Serpens Star-forming Region

Law¹,

Ricci²,

Andrews³

et al. 2017

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“…For our analyses, we use distances of 436 pc for the 4 Serpens regions (Ortiz-León et al 2017), and 300 pc for the Perseus region (Schlafly et al 2014). Both clouds have an average recessional velocity of 7.5 − 8 km/s.…”

Section: Discussionmentioning

confidence: 99%

Morphology and Kinematics of Filaments in the Serpens and Perseus Molecular Clouds

Dhabal

Mundy

Rizzo

et al. 2018

ApJ

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We present H 13 CO + (J=1-0) and HNC (J=1-0) maps of regions in Serpens South, Serpens Main and NGC 1333 containing filaments. We also observe the Serpens regions using H 13 CN (J=1-0). These dense gas tracer molecular line observations carried out with CARMA have an angular resolution of ∼ 7 , a spectral resolution of ∼ 0.16 km/s and a sensitivity of 50-100 mJy/beam. Although the large scale structure compares well with the Herschel dust continuum maps, we resolve finer structure within the filaments identified by Herschel. The H 13 CO + emission distribution agrees with the existing CARMA N 2 H + (J=1-0) maps; so they trace the same morphology and kinematics of the filaments. The H 13 CO + maps additionally reveal that many regions have multiple structures partially overlapping in the line-of-sight. In two regions, the velocity differences are as high as 1.4 km/s. We identify 8 filamentary structures having typical widths of 0.03 − 0.08 pc in these tracers. At least 50% of the filamentary structures have distinct velocity gradients perpendicular to their major axis with average values in the range 4 − 10 km s −1 pc −1 . These findings are in support of the theoretical models of filament formation by 2-D inflow in the shock layer created by colliding turbulent cells. We also find evidence of velocity gradients along the length of two filamentary structures; the gradients suggest that these filaments are inflowing towards the cloud core.

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“…Spatially there appears to be overlap between the stars of Serpens South and W40, which has led to the suggestion of an association between the two (Povich et al 2013). Ortiz-León et al (2017) use VLBA radio parallax data including sources in W40 and claim a distance of 436±9.2 pc for the combined W40+Serpens South region (see also Dzib et al 2011). Conversely, SMA data have been used to provide local standard of rest velocities for the Serpens South members.…”

Section: Serpens Southmentioning

confidence: 99%

YSOVAR: Mid-infrared Variability among YSOs in the Star Formation Region Serpens South

Wolk

Günther

Poppenhaeger

et al. 2018

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We present a time-variability study of young stellar objects (YSOs) in the Serpens South cluster performed at 3.6 and 4.5 μm with the Spitzer Space Telescope; this study is part of the Young Stellar Object VARiability project. We have collected light curves for more than 1500 sources, including 85 cluster members, over 38 days. This includes 44 class I sources, 19 sources with flat spectral energy distributions (SEDs), 17 class II sources, and five diskless YSO candidates. We find a high variability fraction among embedded cluster members of ∼70%, whereas young stars without a detectable disk display no variability. We detect periodic variability for 32 sources with periods primarily in the range of 0.2-14 days and a subset of fast rotators thought to be field binaries. The timescale for brightness changes are shortest for stars with the most photospheric SEDs and longest for those with flat or rising SEDs. While most variable YSOs become redder when fainter, as would be expected from variable extinction, about 10% get bluer as they get fainter. One source, SSTYSV J183006.13−020108.0, exhibits "cyclical" color changes.

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The Gould’s Belt Distances Survey (Gobelins). Iii. The Distance to the Serpens/Aquila Molecular Complex

Cited by 130 publications

References 50 publications

An SMA Continuum Survey of Circumstellar Disks in the Serpens Star-forming Region

An SMA Continuum Survey of Circumstellar Disks in the Serpens Star-forming Region

Morphology and Kinematics of Filaments in the Serpens and Perseus Molecular Clouds

YSOVAR: Mid-infrared Variability among YSOs in the Star Formation Region Serpens South

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