A network of filaments detected by<i>Herschel</i>in the Serpens core

Roccatagliata, V.; Dale, James E.; Ratzka, Thorsten; Testi, L.; Burkert, Andreas; Koepferl, Christine; Sicilia‐Aguilar, A.; Eiroa, C.; Gaczkowski, B.

doi:10.1051/0004-6361/201425253

Cited by 16 publications

(28 citation statements)

References 55 publications

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“…Based on the Herschel observations, the Serpens filament is estimated to have a size of ∼0.3 pc×1.7 pc, and a position angle of 147 • east of north (Roccatagliata et al 2015). The highly rectilinear morphology of the Serpens filament is clearly seen in dust emission which matches the 12 µm absorption very well (see Fig.…”

Section: Introductionmentioning

confidence: 84%

“…The Serpens filament, named by Enoch et al (2007), is also known as the "starless cores" region in Burleigh et al (2013) and Filament 9 in Roccatagliata et al (2015). This filament resides in the Serpens cloud, the distance of which is about 440 pc as deduced from the trigonometric parallax measured with the Very Long Baseline Array (VLBA) (Ortiz-León et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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The Serpens filament at the onset of slightly supercritical collapse

Gong¹,

Li²,

Mao³

et al. 2018

A&A

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The Serpens filament, as one of the nearest infrared dark clouds, is regarded as a pristine filament at a very early evolutionary stage of star formation. In order to study its molecular content and dynamical state, we mapped this filament in seven species including C 18 O, HCO + , HNC, HCN, N 2 H + , CS, and CH 3 OH. Among them, HCO + , HNC, HCN, and CS show self-absorption, while C 18 O is most sensitive to the filamentary structure. A kinematic analysis demonstrates that this filament forms a velocity-coherent (trans-)sonic structure, a large part of which is one of the most quiescent regions in the Serpens cloud. Widespread C 18 O depletion is found throughout the Serpens filament. Based on the Herschel dust-derived H 2 column density map, the line mass of the filament is 36-41 M ⊙ pc −1 , and its full width at half maximum width is 0.17±0.01 pc, while its length is ≈ 1.6 pc. The inner radial column density profile of this filament can be well fitted with a Plummer profile with an exponent of 2.2±0.1, a scale radius of 0.018 ± 0.003 pc, and a central density of (4.0 ± 0.8) × 10 4 cm −3 . The Serpens filament appears to be slightly supercritical. The widespread blue-skewed HNC and CS line profiles and HCN hyperfine line anomalies across this filament indicate radial infall in parts of the Serpens filament. C 18 O velocity gradients also indicate accretion flows along the filament. The velocity and density structures suggest that such accretion flows are likely due to a longitudinal collapse parallel to the filament's long axis. Both the radial infall rate (∼72 M ⊙ Myr −1 , inferred from HNC and CS blue-skewed profiles) and the longitudinal accretion rate (∼10 M ⊙ Myr −1 , inferred from C 18 O velocity gradients) along the Serpens filament are lower than all previously reported values in other filaments. This indicates that the Serpens filament lies at an early evolutionary stage when collapse has just begun, or that thermal and non-thermal support are effective in providing support against gravity.

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Section: Introductionmentioning

confidence: 84%

Section: Introductionmentioning

confidence: 99%

The Serpens filament at the onset of slightly supercritical collapse

Gong¹,

Li²,

Mao³

et al. 2018

A&A

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“…Both clouds have an average recessional velocity of 7.5 − 8 km/s. Dust temperatures in these filaments range from 12 K to 15 K (Roccatagliata et al 2015;Tanaka et al 2013). We use the Spitzer catalog of YSOs (Dunham et al 2015) and identified point sources in the Herschel 70 µm maps corresponding to the studied regions to compare their locations with respect to the structures identified by us.…”

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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“…Federrath & Klessen 2012;Ward et al 2014;Girichidis et al 2014) and observers (see e.g. Kainulainen et al 2009Kainulainen et al , 2011Palmeirim et al 2013;Tremblin et al 2014;Schneider et al 2015;Roccatagliata et al 2015) use them in their studies and they are a good tool for comparing both simulations and observations with each other. As Lupus I is close to us and lies at a high Galactic latitude far away from the Galactic plane, we expect the contamination of the map by overlaying foreground or background emission to be small.…”

Section: Column Density Pdfsmentioning

confidence: 99%

Squeezed between shells? The origin of the Lupus I molecular cloud

Gaczkowski

Preibisch

Stanke³

et al. 2015

A&A

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Context. The Lupus I cloud is found between the Upper Scorpius (USco) and the Upper Centaurus-Lupus (UCL) subgroups of the Scorpius-Centaurus OB association, where the expanding USco H I shell appears to interact with a bubble currently driven by the winds of the remaining B-stars of UCL. Aims. We want to study how collisions of large-scale interstellar gas flows form and influence new dense clouds in the ISM. Methods. We performed LABOCA continuum sub-mm observations of Lupus I that provide for the first time a direct view of the densest, coldest cloud clumps and cores at high angular resolution. We complemented these data with Herschel and Planck data from which we constructed column density and temperature maps. From the Herschel and LABOCA column density maps we calculated probability density functions (PDFs) to characterize the density structure of the cloud. Results. The northern part of Lupus I is found to have, on average, lower densities, higher temperatures, and no active star formation. The center-south part harbors dozens of pre-stellar cores where density and temperature reach their maximum and minimum, respectively. Our analysis of the column density PDFs from the Herschel data show double-peak profiles for all parts of the cloud, which we attribute to an external compression. In those parts with active star formation, the PDF shows a power-law tail at high densities. The PDFs we calculated from our LABOCA data trace the denser parts of the cloud showing one peak and a power-law tail. With LABOCA we find 15 cores with masses between 0.07 and 1.71 M and a total mass of ≈8 M . The total gas and dust mass of the cloud is ≈164 M and hence ∼5% of the mass is in cores. From the Herschel and Planck data we find a total mass of ≈174 M and ≈171 M , respectively. Conclusions. The position, orientation, and elongated shape of Lupus I, the double-peak PDFs and the population of pre-stellar and protostellar cores could be explained by the large-scale compression from the advancing USco H I shell and the UCL wind bubble.

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A network of filaments detected byHerschelin the Serpens core

Cited by 16 publications

References 55 publications

The Serpens filament at the onset of slightly supercritical collapse

The Serpens filament at the onset of slightly supercritical collapse

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

Squeezed between shells? The origin of the Lupus I molecular cloud

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