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J/MNRAS/475/2003    Red supergiant population in Perseus arm     (Dorda+, 2018)

The red supergiant population in the Perseus arm. Dorda R., Negueruela I., Gonzalez-Fernandez C. <Mon. Not. R. Astron. Soc. 475, 2003 (2018)> =2018MNRAS.475.2003D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, late-type ; Stars, supergiant ; Stars, luminous ; MK spectral classification Keywords: stars: late-type - stars: massive - supergiants - open clusters and associations: general - Galaxy: stellar content Abstract: We present a new catalogue of cool supergiants in a section of the Perseus arm, most of which had not been previously identified. To generate it, we have used a set of well-defined photometric criteria to select a large number of candidates (637) that were later observed at intermediate resolution in the infrared calcium triplet spectral range, using a long-slit spectrograph. To separate red supergiants from luminous red giants, we used a statistical method, developed in previous works and improved in the present paper. We present a method to assign probabilities of being a red supergiant to a given spectrum and use the properties of a population to generate clean samples, without contamination from lower luminosity stars. We compare our identification with a classification done using classical criteria and discuss their respective efficiencies and contaminations as identification methods. We confirm that our method is as efficient at finding supergiants as the best classical methods, but with a far lower contamination by red giants than any other method. The result is a catalogue with 197 cool supergiants, 191 of which did not appear in previous lists of red supergiants. This is the largest coherent catalogue of cool supergiants in the Galaxy. Description: The targets were observed during two different campaigns. The first one was done in 2011, on the nights of October 16-18. The second campaign was carried out in 2012, from September 3rd to 7th. We used the Intermediate Dispersion Spectrograph, mounted on the 2.5 m Isaac Newton Telescope (INT) in La Palma (Spain). In total, we observed 637 unique targets, 102 in 2011 and 535 in 2012, without any overlap between epochs. As discussed above, 43 of them are CSGs with well-determined SpTs (all but one observed in the 2012 run) that were included in the calibration sample of Paper III (see appendix B in that work). These objects are not considered part of the Perseus sample studied here. This leaves 594 targets in our sample, which are detailed in perseus.dat file. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file perseus.dat 65 594 Catalogue of targets observed in the Perseus arm
See also: J/A+A/578/A3 : New survey of supergiants in the MCs (Gonzalez-Fernandez+, 2015) Byte-by-byte Description of file: perseus.dat
Bytes Format Units Label Explanations
1- 6 A6 --- ID Designation (PERNNN) 8- 9 I2 h RAh Right Ascension (Eq=J2000, Ep= 1989.0) 11- 12 I2 min RAm Right Ascension (Eq=J2000, Ep= 1989.0) 14- 18 F5.2 s RAs Right Ascension (Eq=J2000, Ep= 1989.0) 20 A1 --- DE- Declination sign (Eq=J2000, Ep= 1989.0) 21- 22 I2 deg DEd Declination (Eq=J2000, Ep= 1989.0) 24- 25 I2 arcmin DEm Declination (Eq=J2000, Ep= 1989.0) 27- 30 F4.1 arcsec DEs Declination (Eq=J2000, Ep= 1989.0) 32- 35 I4 yr Ep.Obs Epoch in which it was observed 37- 40 A4 --- SpType Spectral type assigned 42- 47 A6 --- LC Luminosity class assigned 49- 53 F5.3 --- P(PCA) ? Probability of being a CSG calculated through the PCA method 55- 59 F5.3 --- P(CaT) ? Probability of being a CSG calculated through the CaT criterion 61- 65 F5.3 --- P(Ti/Fe) ? Probability of being a CSG calculated through the ratio of Ti-to-Fe criterion
Acknowledgements: Ricardo Dorda, ricardo.dorda(at)ua.es References: Gonzalez-Fernandez et al., Paper I 2015A&A...578A...3G, Cat. J/A+A/578/A3 Dorda et al., Paper II 2016A&A...592A..16D Dorda et al., Paper III 2016A&A...595A.105D
(End) Ricardo Dorda [Univ. Alicante], Patricia Vannier [CDS] 29-Mar-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

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