Interstellar extinction in the area of the Serpens Cauda molecular cloud

Straižys, V.; Cernis, K.; Bartasiute, S.

doi:10.1515/astro-1996-0106

Cited by 68 publications

(109 citation statements)

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“…A distance of 225 ± 55 pc has been derived for this extinction wall, using spectro-photometric studies of the optically visible stars (Straižys et al 2003). This distance is very similar to the usually adopted distance of 260 ± 37 pc for the Serpens star-forming region 1 , located only 3 • north (Straižys et al 1996).…”

Section: Overview and Distance Of The Aquila Rift Complexsupporting

confidence: 87%

TheHerschelfirst look at protostars in the Aquila rift

Bontemps

André

Könyves

et al. 2010

A&A

123

107

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As part of the science demonstration phase of the Herschel mission of the Gould Belt key program, the Aquila rift molecular complex has been observed. The complete ∼3.3 • × 3.3 • imaging with SPIRE 250/350/500 μm and PACS 70/160 μm allows a deep investigation of embedded protostellar phases, probing of the dust emission from warm inner regions at 70 and 160 μm to the bulk of the cold envelopes between 250 and 500 μm. We used a systematic detection technique operating simultaneously on all Herschel bands to build a sample of protostars. Spectral energy distributions are derived to measure luminosities and envelope masses, and to place the protostars in an M env −L bol evolutionary diagram. The spatial distribution of protostars indicates three star-forming sites in Aquila, with W40/Sh2-64 HII region by far the richest. Most of the detected protostars are newly discovered. For a reduced area around the Serpens South cluster, we could compare the Herschel census of protostars with Spitzer results. The Herschel protostars are younger than in Spitzer with 7 Class 0 YSOs newly revealed by Herschel. For the entire Aquila field, we find a total of ∼45-60 Class 0 YSOs discovered by Herschel. This confirms the global statistics of several hundred Class 0 YSOs that should be found in the whole Gould Belt Survey.

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Section: Overview and Distance Of The Aquila Rift Complexsupporting

confidence: 87%

TheHerschelfirst look at protostars in the Aquila rift

Bontemps

André

Könyves

et al. 2010

A&A

123

107

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“…Indeed, assuming that Serpens Main and Aquila rift are different entities also has the advantage of explaining the discrepancy found between their extinction-based distance estimates (Straižys et al 1996(Straižys et al , 2003Bontemps et al 2010;Knude 2011): ∼200-280 pc for the Aquila rift complex (due to the known extinction wall at a distance of 225 ± 55 pc), and ∼415 pc for Serpens Main (from the recent VLBI-based distance by Dzib et al 2010), suggesting that Serpens Main is located behind the extinction wall associated to Serpens South.…”

Section: Distance Of the Star Forming Clouds In The Aquila Riftmentioning

confidence: 99%

The formation of active protoclusters in the Aquila rift: a millimeter continuum view

Maury¹,

André²,

Men’shchikov³

et al. 2011

A&A

129

244

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While most stars are believed to form in stellar clusters, the formation and early evolution of young stellar clusters is still largely unknown. Improving our knowledge of the earliest phases of clustered star formation is crucial for understanding the origin of the stellar initial mass function and the efficiency of the star formation process, which both play a key role in the evolution of galaxies. Here, we present an analysis of the Aquila rift complex which addresses the questions of the star formation rate (SFR), star formation efficiency (SFE) and typical lifetime of the Class 0 protostellar phase in two nearby cluster-forming clumps: the Serpens South and W40 protoclusters. We carried out a 1.2 mm dust continuum mapping of the Aquila rift complex with the MAMBO bolometer array on the IRAM 30 m telescope. Using a multi-scale source extraction method, we perform a systematic source extraction in our millimeter continuum map. Based on complementary data from the Herschel Gould Belt survey and Spitzer maps, we characterize the spectral energy distributions (SEDs) of the 77 mm continuum sources detected with MAMBO and estimate their evolutionary stages. Taking advantage of the comprehensive dataset available for the Serpens South region, spanning wavelengths from 2 μm to 1.2 mm, we estimate the numbers of young stellar objects (YSOs) at different evolutionary stages and find a ratio of Class 0 to Class I protostars N(0)/N(I) = 0.19−0.27. This low ratio supports a scenario of relatively fast accretion at the beginning of the protostellar phase, and leads to a Class 0 lifetime of ∼4−9 × 10 4 yr. We also show that both the Serpens South and W40 protoclusters are characterized by large fractions of protostars and high SFRs ∼ 20−50 M Myr −1 pc −2 , in agreement with the idea that these two nearby clumps are active sites of clustered star formation currently undergoing bursts of star formation, and have the potential ability to form bound star clusters. While the formation of these two protoclusters is likely to have been initiated in a very different manner, the resulting protostellar populations are observed to be very similar. This suggests that after the onset of gravitational collapse, the detailed manner in which the collapse has been initiated does not affect much the ability of a clump to form stars.

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“…At a distance of 100 pc this corresponds to physical sizes of ∼400−500 AU and ∼700−1000 AU, respectively. The clouds observed in the c2d program are assumed to be located at distances A&A 519, A3 (2010) Enoch et al 2006), Taurus-Auriga (160 pc Kenyon et al 1994), Serpens (260 pc Straizys et al 1996). ranging from 125 pc (Ophiuchus) to 260 pc (Serpens) increasing the physical area observed.…”

Section: Separating Disk and Cloud Emission -Optimal Extractionmentioning

confidence: 99%

c2dSpitzerIRS spectra of embedded low-mass young stars: gas-phase emission lines

Lahuis

Dishoeck

Jørgensen

et al. 2010

A&A

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Context. A survey of mid-infrared gas-phase emission lines of H 2 , H 2 O and various atoms toward a sample of 43 embedded low-mass young stars in nearby star-forming regions is presented. The sources are selected from the Spitzer "Cores to Disks" (c2d) legacy program. Aims. The environment of embedded protostars is complex both in its physical structure (envelopes, outflows, jets, protostellar disks) and the physical processes (accretion, irradiation by UV and/or X-rays, excitation through slow and fast shocks) which take place. The mid-IR spectral range hosts a suite of diagnostic lines which can distinguish them. A key point is to spatially resolve the emission in the Spitzer-IRS spectra to separate extended PDR and shock emission from compact source emission associated with the circumstellar disk and jets.Methods. An optimal extraction method is used to separate both spatially unresolved (compact, up to a few hundred AU) and spatially resolved (extended, thousand AU or more) emission from the IRS spectra. The results are compared with the c2d disk sample and literature PDR and shock models to address the physical nature of the sources. Conclusions. The observed emission on ≥1000 AU scales is characteristic of PDR emission and likely originates in the outflow cavities in the remnant envelope created by the stellar wind and jets from the embedded young stars. Weak shocks along the outflow wall can also contribute. The compact emission is likely of mixed origin, comprised of optically thick circumstellar disk and/or jet/outflow emission from the protostellar object.

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Interstellar extinction in the area of the Serpens Cauda molecular cloud

Cited by 68 publications

References 0 publications

TheHerschelfirst look at protostars in the Aquila rift

TheHerschelfirst look at protostars in the Aquila rift

The formation of active protoclusters in the Aquila rift: a millimeter continuum view

c2dSpitzerIRS spectra of embedded low-mass young stars: gas-phase emission lines

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