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J/A+A/606/A142      L1544 1.2 and 2mm emission maps      (Chacon-Tanarro+, 2017)

Search for grain growth towards the center of L1544. Chacon-Tanarro A., Caselli P., Bizzocchi L., Pineda J.E., Harju J., Spaans M., Desert F.-X. <Astron. Astrophys. 606, A142 (2017)> =2017A&A...606A.142C (SIMBAD/NED BibCode)
ADC_Keywords: Radio continuum ; Molecular clouds Keywords: ISM: clouds - ISM: individual objects: L1544 - ISM: dust, extinction - opacity - stars: formation Abstract: In dense and cold molecular clouds dust grains are surrounded by thick icy mantles. It is however not clear if dust growth and coagulation take place before the switch-on of a protostar. This is an important issue, as the presence of large grains may affect the chemical structure of dense cloud cores, including the dynamically important ionization fraction, and the future evolution of solids in protoplanetary disks. To study this further, we focus on L1544, one of the most centrally concentrated pre-stellar cores on the verge of star formation, and with a well-known physical structure. We observed L1544 at 1.2 and 2mm using NIKA, a new receiver at the IRAM 30 m telescope, and we used data from the Herschel Space Observatory archive. We find no evidence of grain growth towards the center of L1544 at the available angular resolution. Therefore, we conclude that single dish observations do not allow us to investigate grain growth towards the pre-stellar core L1544 and high sensitivity interferometer observations are needed. We predict that dust grains can grow to 200um in size toward the central ∼300au of L1544. This will imply a dust opacity change by a factor of ∼2.5 at 1.2mm, which can be detected using the Atacama Large Millimeter and submillimeter Array (ALMA) at different wavelengths and with an angular resolution of 2". Description: Millimeter observations of the pre-stellar core L1544 are presented. These observations were carried out at the IRAM 30m telescope, located at Pico Veleta (Spain) using the New IRAM KID Array (NIKA). The project number is 151-13. A region of 3°x3° was mapped using the Lissajous pattern at 1.2 and 2mm. The main beam widths are 12.5-arcsec at 1.2mm and 18.5 arcsec at 2mm. The KID array has a field-of-view is 1.8' at 1.2mm and 2.0' at 2mm. Objects: ----------------------------------------- RA (2000) DE Designation(s) ----------------------------------------- 05 04 18 +25 11.1 L1544 = LDN 1544 ----------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 81 2 List of fitd maps fits/* 0 2 Individual fits maps
See also: J/A+A/555/A109 : 14N/15N isotopic ratio in L1544 (Bizzocchi+, 2013) J/A+A/606/A82 : Observed chemical structure of L1544 (Spezzano+, 2017) J/ApJ/833/176 : The magnetic field of L1544. I. NIR data (Clemens+, 2016) Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000) 10- 18 F9.5 deg DEdeg Declination of center (J2000) 20- 21 I2 --- Nx Number of pixels along X-axis 23- 24 I2 --- Ny Number of pixels along Y-axis 26- 28 I3 Kibyte size Size of FITS file 30- 53 A24 --- FileName Name of FITS file, in subdirectory fits 55- 81 A27 --- Title Title of the FITS file
Acknowledgements: Ana Chacon-Tanarro, achacon(at)mpe.mpg.de
(End) Ana Chacon-Tanarro [MPE, Germany], Patricia Vannier [CDS] 10-Jul-2017
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

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