Access to Astronomical Catalogues

← Click to display the menu
J/ApJ/847/92  Polarization data toward the protostar Serpens SMM1  (Hull+, 2017)

ALMA observations of dust polarization and molecular line emission from the class 0 protostellar source Serpens SMM1. Hull C.L.H., Girart J.M., Tychoniec L., Rao R., Cortes P.C., Pokhrel R., Zhang Q., Houde M., Dunham M.M., Kristensen L.E., Lai S.-P., Li Z.-Y., Plambeck R.L. <Astrophys. J., 847, 92 (2017)> =2017ApJ...847...92H
ADC_Keywords: Polarization; Millimetric/submm sources; Interstellar medium; YSOs Keywords: ISM: jets and outflows ; ISM: magnetic fields ; polarization ; stars: formation ; stars: magnetic field ; stars: protostars Abstract: We present high angular resolution dust polarization and molecular line observations carried out with the Atacama Large Millimeter/submillimeter Array (ALMA) toward the Class 0 protostar Serpens SMM1. By complementing these observations with new polarization observations from the Submillimeter Array (SMA) and archival data from the Combined Array for Research in Millimeter- wave Astronomy (CARMA) and the James Clerk Maxwell Telescopes (JCMT), we can compare the magnetic field orientations at different spatial scales. We find major changes in the magnetic field orientation between large (∼0.1pc) scales-where the magnetic field is oriented E-W, perpendicular to the major axis of the dusty filament where SMM1 is embedded-and the intermediate and small scales probed by CARMA (∼1000au resolution), the SMA (∼350au resolution), and ALMA (∼140au resolution). The ALMA maps reveal that the redshifted lobe of the bipolar outflow is shaping the magnetic field in SMM1 on the southeast side of the source; however, on the northwestern side and elsewhere in the source, low-velocity shocks may be causing the observed chaotic magnetic field pattern. High-spatial-resolution continuum and spectral-line observations also reveal a tight (∼130au) protobinary system in SMM1-b, the eastern component of which is launching an extremely high-velocity, one-sided jet visible in both CO(J=2->1) and SiO(J=5->4); however, that jet does not appear to be shaping the magnetic field. These observations show that with the sensitivity and resolution of ALMA, we can now begin to understand the role that feedback (e.g., from protostellar outflows) plays in shaping the magnetic field in very young, star-forming sources like SMM1. Description: We present ALMA 343GHz (Band 7; 870um) polarization observations toward the very embedded intermediate-mass protostar Serpens SMM1. We complement these observations with new Submillimeter Array (SMA) 345GHz (880um) dust polarization observations as well as with archival polarization maps obtained with the James Clerk Maxwell Telescope (JCMT; 850um) and the Combined Array for Research in Millimeter-wave Astronomy (CARMA; 1.3mm). The 870um ALMA dust polarization observations that we present were taken on 2015 June 3 and 7, and have a synthesized beam (resolution element) of ∼0.33", corresponding to a linear resolution of ∼140au at a distance of 436pc. We also present 1.3mm (Band 6) ALMA spectral-line data, which were taken in two different array configurations on 2014 August 18 (∼0.3" angular resolution) and 2015 April 06 (∼1" resolution). Finally, we present 1.3mm ALMA continuum data with ∼0.1" resolution (R. Pokhrel et al. 2017, in preparation), observed on 2016 September 10, 13, and 2016 October 31. The SMA polarization observations (Figure 1(c)) were taken on 2012 May 25 (compact configuration) and 2012 September 2 and 3 (extended configuration), and have a synthesized beam of ∼0.8". The archival JCMT SCUBA polarization data (Figure 1(a)) were obtained from supplementary data provided by Matthews+ (2009, J/ApJS/182/143). The CARMA polarization data (Figure 1(b)) were taken between 2011 and 2013 as part of the TADPOL survey (Hull+ 2014, J/ApJS/213/13). The data were taken using the 1.3mm polarization receiver system in the C, D, and E arrays at CARMA, which correspond to angular resolutions at 1.3mm of approximately 1", 2", and 4", respectively. Objects: --------------------------------------------------------------- RA (ICRS) DE Designation(s) --------------------------------------------------------------- 18 29 49.63 +01 15 21.9 Serpens SMM1 = NAME Serpens SMM 1 --------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 36 4 SMM1 source properties table3.dat 42 383 ALMA polarization data
See also: J/ApJ/707/103 : Observation of Ser FIRS 1 at 230GHz (Enoch+, 2009) J/A+A/563/L3 : NGC1333-IRAS2A CALYPSO IRAM-PdBI SiO & SO maps (Codella+, 2014) J/ApJ/783/6 : Deconvolved Spitzer images of 89 protostars (Velusamy+, 2014) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Name Source name 8- 9 I2 h RAh [18] Hour of right ascension (J2000) 11- 12 I2 min RAm [29] Minute of right ascension (J2000) 14- 18 F5.2 s RAs [49.6/50] Second of right ascension (J2000) 20 A1 --- DE- [+] Sign of declination (J2000) 21 I1 deg DEd [1] Degree of declination (J2000) 23- 24 I2 arcmin DEm [15] Arcminute of declination (J2000) 26- 30 F5.2 arcsec DEs [20.4/23] Arcsecond of declination (J2000) 32- 36 F5.1 mJy/beam I870 [10/800] Peak intensity of each of the sources in the 870um ALMA data
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 9 F9.5 deg RAdeg [277.456/277.459] Right Ascension (J2000) 11- 17 F7.5 deg DEdeg [1.254/1.258] Declination (J2000) 19- 23 F5.1 deg chi Polarization position angle 25- 27 F3.1 deg e_chi [0.2/9.5] Uncertainty in chi 29- 34 F6.3 mJy/beam Pol [0.18/10.86] Polarized intensity 36- 42 F7.3 mJy/beam Int [1.5/745]? Total intensity (1)
Note (1): Reported where I>3σ. Due to differences in dynamic range between the images of Stokes I and polarized intensity, there are cases where Pol is detectable but I is not.
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 31-May-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© Unistra/CNRS

Contact