A submillimetre survey of the kinematics of the Perseus molecular cloud â I. Data

Curtis, Emily I.; Richer, J. S.; Buckle, Jane

doi:10.1111/j.1365-2966.2009.15658.x

Cited by 53 publications

(74 citation statements)

References 88 publications

(145 reference statements)

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“…For example, observations of the Perseus molecular cloud give α values of −0.36 ± 0.08 (0.1 < M/M⊙ < 3) and −0.4 ± 0.2 (0.03 < M/M⊙ < 5) for C 18 O(3-2) and 13 CO(3-2) (Curtis 2009), respectively, both of which are consistent with our estimate based on dust emission for the mass ranges in common. The maps of C 18 O are, in fact, strikingly similar to those in the 850 µm continuum (Curtis et al 2010), suggesting that similar densities of material are being traced. It seems likely, therefore, that our unbound starless cores represent the dust-emission counterparts of the C 18 O clumps.…”

Section: Overall Starless Core Mass Functionmentioning

confidence: 58%

A census of dense cores in the Taurus L1495 cloud from theHerschelGould Belt Survey

Marsh

Kirk

André

et al. 2016

Mon. Not. R. Astron. Soc.

121

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We present a catalogue of dense cores in a ∼ 4 • × 2 • field of the Taurus star-forming region, inclusive of the L1495 cloud, derived from Herschel SPIRE and PACS observations in the 70 µm, 160 µm, 250 µm, 350 µm, and 500 µm continuum bands. Estimates of mean dust temperature and total mass are derived using modified blackbody fits to the spectral energy distributions. We detect 525 starless cores of which ∼ 10-20% are gravitationally bound and therefore presumably prestellar. Our census of unbound objects is ∼ 85% complete for M > 0.015 M ⊙ in low density regions (A V < ∼ 5 mag), while the bound (prestellar) subset is ∼ 85% complete for M > 0.1 M ⊙ overall. The prestellar core mass function (CMF) is consistent with lognormal form, resembling the stellar system initial mass function, as has been reported previously. All of the inferred prestellar cores lie on filamentary structures whose column densities exceed the expected threshold for filamentary collapse, in agreement with previous reports. Unlike the prestellar CMF, the unbound starless CMF is not lognormal, but instead is consistent with a power-law form below 0.3 M ⊙ and shows no evidence for a lowmass turnover. It resembles previously reported mass distributions for CO clumps at low masses (M < ∼ 0.3 M ⊙ ). The volume density PDF, however, is accurately lognormal except at high densities. It is consistent with the effects of self-gravity on magnetized supersonic turbulence. The only significant deviation from lognormality is a high-density tail which can be attributed unambiguously to prestellar cores.

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Section: Overall Starless Core Mass Functionmentioning

confidence: 58%

A census of dense cores in the Taurus L1495 cloud from theHerschelGould Belt Survey

Marsh

Kirk

André

et al. 2016

Mon. Not. R. Astron. Soc.

121

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“…The data used is C 18 O J = 3 → 2, at 329.330 GHz, with 0.055 km s −1 spectral resolution, and 14 spatial resolution. The telescope main beam efficiency at this frequency is η mb = 0.66 (Curtis et al 2010), and the rms level achieved is of the order of 0.2 K (T A ). A full description of these data is given in the GBS Serpens First Look paper (Graves et al 2010, hereafter referred to as SFLPaper).…”

Section: Jcmt Datamentioning

confidence: 89%

The physical and dynamical structure of Serpens

Duarte-Cabral¹,

Fuller²,

Peretto³

et al. 2010

A&A

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Context. The Serpens North cluster is a nearby low mass star forming region which is part of the Gould belt. It contains a range of young stars thought to correspond to two different bursts of star formation and provides the opportunity to study different stages of cluster formation. Aims. This work aims to study the molecular gas in the Serpens North cluster to probe the origin of the most recent burst of star formation in Serpens. Methods. Transitions of the C 17 O and C 18 O observed with the IRAM 30 m telescope and JCMT are used to study the mass and velocity structure of the region while the physical properties of the gas are derived using LTE and non-LTE analyses of the three lowest transitions of C 18 O. Results. The molecular emission traces the two centres of star formation which are seen in submillimetre dust continuum emission. In the ∼40 M NW sub-cluster the gas and dust emission trace the same structures although there is evidence of some depletion of the gas phase C 18 O. The gas has a very uniform temperature (∼10 K) and velocity (∼8.5 km s −1 ) throughout the region. This is in marked contrast to the SE sub-cluster. In this region the dust and the gas trace different features, with the temperature peaking between the submillimetre continuum sources, reaching up to ∼14 K. The gas in this region has double peaked line profiles which reveal the presence of a second cloud in the line of sight. The submillimetre dust continuum sources predominantly appear located in the interface region between the two clouds. Conclusions. Even though they are at a similar stage of evolution, the two Serpens sub-clusters have very different characteristics. We propose that these differences are linked to the initial trigger of the collapse in the regions and suggest that a cloud-cloud collision could explain the observed properties.

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“…The companion to IRAS 4B is clearly detected at a separation of 11 , whereas that of IRAS 4A has a separation of only 2 (Jørgensen et al 2007). The distance to the NGC 1333 nebula remains unclear (see Curtis et al 2010a, for more thorough discussions). In this paper, we adopt the distance of 235 ± 18 pc based on VLBI parallax measurements of water masers in SVS 13 in the same cluster (Hirota et al 2008).…”

Section: Introductionmentioning

confidence: 99%

APEX-CHAMP⁺high-JCO observations of low-mass young stellar objects

Yıldız

Kristensen

Dishoeck

et al. 2012

A&A

109

243

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Context. The NGC 1333 IRAS 4A and IRAS 4B sources are among the most well-studied Stage 0 low-mass protostars, which drive prominent bipolar outflows. Spectrally resolved molecular emission lines provide crucial information about the physical and chemical structure of the circumstellar material as well as the dynamics of the different components. Most studies have so far concentrated on the colder parts (T ≤ 30 K) of these regions. Aims. The aim is to characterize the warmer parts of the protostellar envelope using the new generation of submillimeter instruments. This will allow us to quantify the feedback of the protostars on their surroundings in terms of shocks, ultraviolet (UV) heating, photodissociation, and outflow dispersal. Methods. The dual frequency 2 × 7 pixel 650/850 GHz array receiver CHAMP + mounted on APEX was used to obtain a fully sampled, large-scale ∼4 × 4 map at 9 resolution of the IRAS 4A/4B region in the 12 CO J = 6-5 line. Smaller maps were observed in the 13 CO 6-5 and [C i] J = 2-1 lines. In addition, a fully sampled 12 CO J = 3-2 map made with HARP-B on the JCMT is presented and deep isotopolog observations are obtained at selected outflow positions to constrain the optical depth. Complementary Herschel-HIFI and ground-based lines of CO and its isotopologs, from J = 1-0 up to 10-9 (E u /k ≈ 300 K), are collected at the source positions and used to construct velocity-resolved CO ladders and rotational diagrams. Radiative-transfer models of the dust and lines are used to determine the temperatures and masses of the outflowing and photon-heated gas and infer the CO abundance structure. Results. Broad CO emission-line profiles trace entrained shocked gas along the outflow walls, which have an average temperature of ∼100 K. At other positions surrounding the outflow and the protostar, the 6-5 line profiles are narrow indicating UV excitation. The narrow 13 CO 6-5 data directly reveal the UV heated gas distribution for the first time. The amount of UV-photon-heated gas and outflowing gas are quantified from the combined 12 CO and 13 CO 6-5 maps and found to be comparable within a 20 radius around IRAS 4A, which implies that UV photons can affect the gas as much as the outflows. Weak [C I] emission throughout the region indicates that there is a lack of CO dissociating photons. Our modeling of the C 18 O lines demonstrates the necessity of a "drop" abundance profile throughout the envelopes where the CO freezes out and is reloaded back into the gas phase through grain heating, thus providing quantitative evidence of the CO ice evaporation zone around the protostars. The inner abundances are less than the canonical value of CO/H 2 = 2.7 × 10 −4 , however, implying that there is some processing of CO into other species on the grains. The implications of our results for the analysis of spectrally unresolved Herschel data are discussed.

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A submillimetre survey of the kinematics of the Perseus molecular cloud â I. Data

Cited by 53 publications

References 88 publications

A census of dense cores in the Taurus L1495 cloud from theHerschelGould Belt Survey

A census of dense cores in the Taurus L1495 cloud from theHerschelGould Belt Survey

The physical and dynamical structure of Serpens

APEX-CHAMP⁺high-JCO observations of low-mass young stellar objects

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A submillimetre survey of the kinematics of the Perseus molecular cloud â I. Data

Cited by 53 publications

References 88 publications

A census of dense cores in the Taurus L1495 cloud from theHerschelGould Belt Survey

A census of dense cores in the Taurus L1495 cloud from theHerschelGould Belt Survey

The physical and dynamical structure of Serpens

APEX-CHAMP+high-JCO observations of low-mass young stellar objects

Contact Info

Product

Resources

About

A submillimetre survey of the kinematics of the Perseus molecular cloud â I. Data

APEX-CHAMP⁺high-JCO observations of low-mass young stellar objects