J/A+A/550/A62 DIBs from Baade's window bulge clump giants (Chen+, 2013)
Extracting interstellar diffuse absorption bands from cool star spectra.
Application to bulge clump giants in Baade's window.
Chen H.-C., Lallement R., Babusiaux C., Puspitarini L., Bonifacio P.,
Hill V.
<Astron. Astrophys., 550, A62 (2013)>
=2013A&A...550A..62C 2013A&A...550A..62C
ADC_Keywords: Stars, giant; Equivalent widths
Keywords: ISM: lines and bands - dust, extinction - ISM: structure -
ISM: molecules - stars: late-type - methods: data analysis
Abstract:
Interstellar (IS) absorption lines or diffuse bands are usually
extracted from early-type star spectra because they are characterized
by smooth continua. However, this introduces a strong limitation on
the number of available targets, and reduces potential studies of the
IS matter and the use of absorptions for cloud mapping.
We have developed a new and automated fitting method appropriate to
interstellar (IS) absorptions in the spectra of cool stars that
possess stellar atmospheric parameters. We applied this method to the
extraction of three diffuse interstellar bands (DIBs) in high
resolution VLT FLAMES/GIRAFFE spectra of red-clump stars from the
bulge. By combining all stellar synthetic spectra, HITRAN-LBLRTM
atmospheric transmission spectra and diffuse band empirical absorption
profiles, we determined the 6196.0, 6204.5, and 6283.8Å DIB
strength toward the 219 target stars and discuss the sources of
uncertainties. To test the sensitivity of the DIB extraction, we
compared all three results and compared the DIB equivalent widths
(EWs) with the reddening derived from an independent extinction map
based on OGLE photometric data. We also derived the three independent
color excess estimates based on the DIB strengths and average linear
correlation coefficients previously established in the solar
neighborhood and compared with the OGLE photometric results.
Description:
We used the sample of 219 bulge red clump giants of Hill et al. (2011,
Cat. J/A+A/534/A80). Those stars were observed with FLAMES/GIRAFFE at
the VLT and are located within a 12-arcmin radius field in Baade's
Window (l=0.8, b=-4). We used here the spectra obtained with the
GIRAFFE HR13 setup, leading to a resolution of R=22500 and a spectral
coverage spanning 6120 to 6405Å, which contains three well known
diffuse bands.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 70 219 Stellar data and measurement of equivalent widths
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See also:
II/149 : Diffuse Interstellar Band Measurements (Snow+ 1977)
J/MNRAS/358/563 : Diffuse Interstellar Bands in 49 stars (Megier+, 2005)
J/A+A/429/559 : Diffuse Interstellar Bands in NGC 1448 (Sollerman+, 2005)
J/ApJ/705/32 : Diffuse interstellar bands from HD 183143 (Hobbs+, 2009)
J/ApJ/708/1628 : Diffuse interstellar bands. IV. (McCall+, 2010)
J/A+A/544/A136 : Diffuse Interstellar Bands in 150 stars (Raimond+, 2012)
J/A+A/550/A108 : DIB in VLT-FLAMES Tarantula Survey (van Loon+, 2013)
J/A+A/534/A80 : Baade's window bulge clump giants metallicities (Hill+, 2011)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Star [1/219] Star sequential number, as in
Hill et al., 2011, Cat. J/A+A/534/A80
5- 10 I6 --- Ogle OGLE number, BUL-SC45 NNNNNN, from Paczynski
et al., 1999, Cat. J/AcA/49/319
12- 15 I4 K Teff Effective temperature
17- 20 F4.2 [cm/s2] logg Surface gravity
22- 24 F3.1 km/s Vturb Microturbulent velocity
26- 30 F5.2 [Sun] [Fe/H] Metallicity
32- 36 F5.3 mag E(B-V) Colour excess (1)
38- 40 I3 0.1pm W(6196) DIB6196Å equivalent width before correction
42- 43 I2 0.1pm W(6196)c DIB6196Å equivalent width after correction
45- 46 I2 0.1pm e_W(6196)c rms uncertainty on W(6196) and W(6196)c
48- 50 I3 0.1pm W(6204) DIB6204Å equivalent width before correction
52- 54 I3 0.1pm W(6204)c ? DIB6204Å equivalent width after correction
56- 57 I2 0.1pm e_W(6204)c ? rms uncertainty on W(6204) and W(6204)c
59- 62 I4 0.1pm W(6284) DIB6284Å equivalent width before correction
64- 67 I4 0.1pm W(6284)c ? DIB6284Å equivalent width after correction
69- 70 I2 0.1pm e_W(6284)c ? rms uncertainty on W(6284) and W(6284)c
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Note (1): derived from Sumi (2004MNRAS.349..193S 2004MNRAS.349..193S) by interpolation.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 30-Apr-2013