The Rotating Outflow, Envelope, and Disk of the Class-0/I Protostar [Bhb2007]#11 in the Pipe Nebula

Hara, Chihomi; Shimajiri, Yoshito; Tsukagoshi, Takashi; Kurono, Yasutaka; Saigo, Kazuya; Nakamura, Fúmitaka; Saito, Masao; Wilner, David J.; Kawabe, Ryohei

doi:10.1088/0004-637x/771/2/128

Cited by 38 publications

(40 citation statements)

References 51 publications

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“…Furthermore, the detection of protostellar outflows strongly indicates the presence of discs in the earliest stage of protostellar evolution (Arce et al 2007). For this reason, an increasing effort has been made over the last years to directly identify the presence and dynamics of protostellar discs around Class 0 objects, which resulted in the * seifried@ph1.uni-koeln.de detection of several discs around low-and intermediate-mass protostars, which are possibly in Keplerian rotating (Tobin et al 2012;Hara et al 2013;Murillo et al 2013;Sánchez-Monge et al 2013a;Yen et al 2013;Codella et al 2014;Ohashi et al 2014). This is in agreement with previous observations based on SED modelling, which suggest the presence of well-defined, rotationally supported discs (Jørgensen et al 2009;Enoch et al 2011).…”

Section: Introductionsupporting

confidence: 84%

Revealing the dynamics of Class 0 protostellar discs with ALMA

Seifried

Sánchez-Monge

Walch

et al. 2016

Mon. Not. R. Astron. Soc.

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We present synthetic ALMA observations of Keplerian, protostellar discs in the Class 0 stage studying the emission of molecular tracers like 13 CO, C 18 O, HCO + , H 13 CO + , N 2 H + , and H 2 CO. We model the emission of discs around low-and intermediatemass protostars. We show that under optimal observing conditions ALMA is able to detect the discs already in the earliest stage of protostellar evolution, although the emission is often concentrated to the innermost 50 AU. Therefore, a resolution of a few 0.1" might be too low to detect Keplerian discs around Class 0 objects. We also demonstrate that under optimal conditions for edge-on discs Keplerian rotation signatures are recognisable, from which protostellar masses can be inferred. For this we here introduce a new approach, which allows us to determine protostellar masses with higher fidelity than before. Furthermore, we show that it is possible to reveal Keplerian rotation even for strongly inclined discs and that ALMA should be able to detect possible signs of fragmentation in face-on discs. In order to give some guidance for future ALMA observations, we investigate the influence of varying observing conditions and source distances. We show that it is possible to probe Keplerian rotation in inclined discs with an observing time of 2 h and a resolution of 0.1", even in the case of moderate weather conditions. Furthermore, we demonstrate that under optimal conditions, Keplerian discs around intermediate-mass protostars should be detectable up to kpc-distances.

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Section: Introductionsupporting

confidence: 84%

Revealing the dynamics of Class 0 protostellar discs with ALMA

Seifried

Sánchez-Monge

Walch

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Only L328-IRS (Lee et al 2009(Lee et al , 2013 has L bol , T bol , and envelope mass comparable to those in SMM2E. These two objects are very similar, not only in Hara et al (2013) and Duarte-Cabral et al (2013). Green squares correspond to Very Low Luminosity Objects (VeLLOs), and magenta diamonds correspond to First Hydrostatic Cores (FHCs, see references in Table 4).…”

Section: Comparison Of Smm2e With Other Proto-bd Candidates and Youngmentioning

confidence: 92%

“…7 we plot the outflow force of SMM2E and its bolometric luminosity on data from the literature of outflows observed with interferometers (using similar configurations), in order to avoid estimates of the missing flux which are necessarily uncertain. For the low and intermediate-mass young stellar objects, we used the compilation by Beltran et al (2008), and added the works of Palau et al (2006), Chen et al (2012), Hara et al (2013), andDuarte-Cabral et al (2013). For the lower mass objects we mainly included the VeLLOs and FHCs whose outflow has been detected with an interferometer 3 (L1521F: Bourke et al 2006, Takahashi et al 2013L1148-IRS: Kauffmann et al 2011L1014-IRS: Bourke et al 2005, Maheswar et al 2011L1448-IRS2E: Chen et al 2010Per-Bolo58: Enoch et al 2010, Dunham et al 2011L1451mm: Pineda et al 2011CB17-MMS and CB17-IRS: Chen et al 2012).…”

Section: Comparison Of Smm2e With Other Proto-bd Candidates and Youngmentioning

confidence: 99%

IC 348-SMM2E: a Class 0 proto-brown dwarf candidate forming as a scaled-down version of low-mass stars

Palau¹,

Zapata²,

Rodrı́guez³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We report on Submillimeter Array observations of the 870 µm continuum and CO (3-2), 13 CO (2-1) and C 18 O (2-1) line emission of a faint object, SMM2E, near the driving source of the HH 797 outflow in the IC 348 cluster. The continuum emission shows an unresolved source for which we estimate a mass of gas and dust of 30 M Jup , and the CO (3-2) line reveals a compact bipolar outflow centred on SMM2E, and barely seen also in 13 CO (2-1). In addition, C 18 O (2-1) emission reveals hints of a possible rotating envelope/disk perpendicular to the outflow, for which we infer a dynamical mass of ∼ 16 M Jup . In order to further constrain the accreted mass of the object, we gathered data from Spitzer, Herschel, and new and archive submillimetre observations, and built the Spectral Energy Distribution (SED). The SED can be fitted with one single modified black-body from 70 µm down to 2.1 cm, using a dust temperature of ∼ 24 K, a dust emissivity index of 0.8, and an envelope mass of ∼ 35 M Jup . The bolometric luminosity is 0.10 L ⊙ , and the bolometric temperature is 35 K. Thus, SMM2E is comparable to the known Class 0 objects in the stellar domain. An estimate of the final mass indicates that SMM2E will most likely remain substellar, and the SMM2E outflow force matches the trend with luminosity known for young stellar objects. Thus, SMM2E constitutes an excellent example of a Class 0 proto-brown dwarf candidate which forms as a scaled-down version of low-mass stars. Finally, SMM2E seems to be part of a wide (∼ 2400 AU) multiple system of Class 0 sources.

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“…Hence, it is interesting to explore the possibility of outflow rotation. In fact, rotation of outflow and jet is suggested for various protostellar sources (Codella et al 2007;Coffey et al 2007;Lee et al 2007Lee et al , 2008Lee et al , 2009Launhardt et al 2009;Zapata et al 2010;Choi et al 2011;Pech et al 2012;Hara et al 2013). Rotation is mostly observed for a collimated jet, while rotation of a well spread outflow like the L1527 outflow is not very evident (B59#11 : Hara et al 2013).…”

Section: Angular Momentummentioning

confidence: 99%

Geometric and Kinematic Structure of the Outflow/Envelope System of L1527 Revealed by Subarcsecond-Resolution Observation of Cs

Oya

Sakai

Leflóch

et al. 2015

ApJ

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Subarcsecond-resolution images of the rotational line emissions of CS and c-C 3 H 2 obtained toward the low-mass protostar IRAS 04368+2557 in L1527 with the Atacama Large Millimeter/submillimeter Array are investigated to constrain the orientation of the outflow/envelope system. The distribution of CS consists of an envelope component extending from north to south and a faint butterfly shaped outflow component. The kinematic structure of the envelope is well reproduced by a simple ballistic model of an infalling rotating envelope. Although the envelope has a nearly edge-on configuration, we find that the western side of the envelope faces the observer. This configuration is opposite to the direction of the large-scale (∼10 4 AU) outflow suggested previously from the 12 CO (J = 3-2) observation, and to the morphology of infrared reflection near the protostar (∼200 AU). The latter discrepancy could originate from high extinction by the outflow cavity of the western side, or may indicate that the outflow axis is not parallel to the rotation axis of the envelope. Position-velocity diagrams show the accelerated outflow cavity wall, and its kinematic structure in the 2000 AU scale is explained by a standard parabolic model with the inclination angle derived from the analysis of the envelope. The different orientation of the outflow between the small and large scale implies a possibility of precession of the outflow axis. The shape and the velocity of the outflow in the vicinity of the protostar are compared with those of other protostars.

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The Rotating Outflow, Envelope, and Disk of the Class-0/I Protostar [Bhb2007]#11 in the Pipe Nebula

Cited by 38 publications

References 51 publications

Revealing the dynamics of Class 0 protostellar discs with ALMA

Revealing the dynamics of Class 0 protostellar discs with ALMA

IC 348-SMM2E: a Class 0 proto-brown dwarf candidate forming as a scaled-down version of low-mass stars

Geometric and Kinematic Structure of the Outflow/Envelope System of L1527 Revealed by Subarcsecond-Resolution Observation of Cs

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