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J/A+A/530/A90    Optically bright post-AGB population of LMC (van Aarle+, 2011)

The optically bright post-AGB population of the LMC. van Aarle E., Van Winckel H., Lloyd Evans T., Ueta T., Wood P.R., Ginsburg A.G. <Astron. Astrophys. 530, A90 (2011)> =2011A&A...530A..90V
ADC_Keywords: Magellanic Clouds ; Stars, giant ; Photometry, UBVRI ; Photometry, infrared ; Photometry, millimetric/submm Keywords: stars: AGB and post-AGB - stars: evolution - Magellanic Clouds - circumstellar matter Abstract: We construct a catalogue of the optically bright post-AGB stars in the LMC. The sample forms an ideal testbed for stellar evolution theory predictions of the final phase of low- and intermediate-mass stars, because the distance and hence luminosity and also the current and initial mass of these objects is well constrained. Description: The paper contains 4 catalogues that are archived electronically: The first and most important one is the catalogue of 70 high probability and 1422 candidate optically bright post-AGB stars in the LMC. For this, we performed a cross-correlation with three optical catalogues and data from 2MASS and SAGE. The estimated luminosity and some cross-correlation remarks with catalogues of other types of objects that have a chance of occuring in our catalogue are also listed. For the 70 objects for which we obtained a spectrum we also give the spectral type and some information on the variability of the source. This catalogue offers strong potential in the study of mass-dependant properties of post-AGB stars such as AGB nucleosynthetic yields via photospheric abundances studies, and mass-loss rates by the distribution of post-AGB stars in the HR diagram. One additional catalogue lists objects for which a low-resolution optical spectrum was obtained, but that are no longer part of our final catalogue of post-AGB candidates. Part of this catalogue appears as an online table in the article, but some extra information is listed here. The last two catalogues contain objects that were discarded based on their too high or too low luminosity but that may be of interest for people studying respectively supergiants or young stellar objects in the LMC as they show similar IR colours. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file cat_pagb.dat 606 1407 Post-AGB candidates cat_spec.dat 606 89 Discarded objects with a spectral type cat_yso.dat 606 6823 Discarded possible YSOs cat_sg.dat 606 286 Discarded possible supergiants
See also: I/305 : The Guide Star Catalog, Version 2.3.2 (GSC2.3) (STScI, 2006) II/236 : UBVR CCD survey of the Magellanic clouds (Massey+, 2002) II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) Byte-by-byte Description of file: cat_*.dat
Bytes Format Units Label Explanations
1- 19 A19 --- Name Name (IRAC, 22- 31 F10.6 deg RAdeg Right ascension (J2000) 34- 43 F10.6 deg DEdeg Declination (J2000) 46- 58 A13 --- Type SED type (cat_pagb and cat_spec only) 60- 68 F9.3 mag Umagz ? Apparent U magnitude from Zaritsky et al. (2004AJ....128.1606Z ) 70- 78 F9.3 mag e_Umagz ? Mean error on Umagz 80- 88 F9.2 mag Umagm ? Apparent U magnitude from Massey (2002, Cat II/236) 90- 98 F9.2 mag e_Umagm ? Mean error on Umagm 100-108 F9.3 mag Bmagz ? Apparent B magnitude from Zaritsky et al. (2004AJ....128.1606Z) 110-118 F9.3 mag e_Bmagz ? Mean error on Bmagz 120-128 F9.2 mag Bmagm ? Apparent B magnitude from Massey (2002, Cat II/236) 130-138 F9.2 mag e_Bmagm ? Mean error on Bmagm 140-148 F9.2 mag Bmagg ? Apparent B magnitude from GSC 2.3.2 (I/305) 150-158 F9.2 mag e_Bmagg ? Mean error on Bmagg 160-168 F9.3 mag Vmagz ? Apparent V magnitude from Zaritsky et al. (2004AJ....128.1606Z) 170-178 F9.3 mag e_Vmagz ? Mean error on Vmagz 180-188 F9.2 mag Vmagm ? Apparent V magnitude from Massey (2002, Cat II/236) 190-198 F9.2 mag e_Vmagm ? Mean error on Vmagm 200-208 F9.2 mag Vmagg ? Apparent V magnitude from GSC 2.3.2 (I/305) 210-218 F9.2 mag e_Vmagg ? Mean error on Vmagg 220-228 F9.2 mag Rmagm ? Apparent R magnitude from Massey (2002, Cat II/236) 230-238 F9.2 mag e_Rmagm ? Mean error on Rmagm 240-248 F9.2 mag Rfmagg ? Apparent Rf magnitude from GSC 2.3.2 (I/305) 250-258 F9.2 mag e_Rfmagg ? Mean error on Rfmagg 260-268 F9.3 mag Imagz ? Apparent I magnitude from Zaritsky et al. (2004AJ....128.1606Z) 270-278 F9.3 mag e_Imagz ? Mean error on Imagz 280-288 F9.3 mag Jmag ? 2MASS J apparent magnitude (II/246) 290-298 F9.3 mag e_Jmag ? Mean error on Jmag 300-308 F9.3 mag Hmag ? 2MASS H apparent magnitude (II/246) 310-318 F9.3 mag e_Hmag ? Mean error on Hmag 320-328 F9.3 mag Kmag ? 2MASS Ks apparent magnitude (II/246) 330-338 F9.3 mag e_Kmag ? Mean error on Kmag 340-348 F9.3 mJy F3.6 ? Spitzer/IRAC 3.6 micron flux 350-358 F9.3 mJy e_F3.6 ? Mean error on F3.6 360-368 F9.3 mJy F4.5 ? Spitzer/IRAC 4.5 micron flux 370-378 F9.3 mJy e_F4.5 ? Mean error on F4.5 380-388 F9.3 mJy F5.8 ? Spitzer/IRAC 5.8 micron flux 390-398 F9.3 mJy e_F5.8 ? Mean error on F5.8 400-408 F9.3 mJy F8.0 ? Spitzer/IRAC 8.0 micron flux 410-418 F9.3 mJy e_F8.0 ? Mean error on F8.0 420-428 F9.4 mJy F24 ? Spitzer/MIPS 24 micron flux 430-438 F9.4 mJy e_F24 ? Mean error on F24 440-448 F9.2 mJy F70 ? Spitzer/MIPS 70 micron flux 450-458 F9.3 mJy e_F70 ? Mean error on F70 460-468 F9.1 mJy F160 ? Spitzer/MIPS 160 micron flux 470-478 F9.2 mJy e_F160 ? Mean error on F160 480-486 I7 solLum LumBB ? Black-body-based luminosity (cat_pag and cat_spec) or Estimated luminosity (cat_sg and cat_yso) 488-494 I7 solLum LumSED ? SED-based luminosity (1) 496-502 I7 solLum e_LumSED ? Mean error on LumSED (1) 504-510 I7 K TeffSED ? SED-based effective temperature (1) 512-518 I7 K e_TeffSED ? Mean error on TeffSED (1) 520-526 F7.2 mag E(B-V) ? SED-based E(B-V) (1) 528-534 F7.2 mag e_E(B-V) ? Mean error on E(B-V) (1) 536-542 A7 --- Xcat ? Cross-correlation with catalogues of other types of objects (1) (3) 544-573 A30 --- SpType ? MK spectral type (1) (4) 575-604 A30 --- Var ? Variability remarks (1) (5) 606 A1 --- n_Name Reason why this object was discarded from our post-AGB sample (2)
Note (1): For cat_pagb and cat_spec only. Note (2): Reason codes as follows (for cat_spec only): A = Not in the current version of the SAGE catalogue B = Does not obey the colour criterion C = Does not survive the black-body luminosity-cut (Sect. 2.3) D = Is listed as a cool carbon star by Kontizas et al. (2001, Cat. J/A+A/369/932) or an AGB star with spectral type by Trams et al. (1999A&A...346..843T) E = Is not a post-AGB star according to the spectral type F = Does not survive the SED luminosity-cut (Sect. 4.1) Note (3): Empirically confirmed cross-matches of the object in the catalogues of Sect. 5.1.3 with A = the RVT stars listed in the recent OGLE-III Catalogue of Variable Stars (Soszynski et al., 2008, Cat J/AcA/58/293) B = the RCrB stars in Soszynski et al. (2009, Cat J/AcA/59/335) C = the MSX post-AGB stars of Wood & Cohen (2001ASSL..265...71W) D = the YSOs from Seale et al. (2009, Cat. J/AJ/699/150) E = the AGB stars from Trams et al. (1999A&A...346..843T) F = the PNe in Reid & Parker (2006, Cat. J/MNRAS/373/521) G = the galaxies in the line of sight of the LMC from NED Note (4): All spectral types indicated with (A) were found in the catalogue of massive stars of Bonanos et al. (2009AJ....138.1003B), the others were determined based on our low-resolution, optical spectra. Note (5): For cat_spec only. The variability remarks are based on both the luminosity curves as discussed in Sect. 5.2 and cross-correlation with the catalogue of Fraser et al. (2008, Cat. J/AJ/136/1242). The latter is indicated with 'Fr_' followed by the correct sequence in subscript. Sequences 9, 0 and -99 indicate subsequently that the star is identified with the One-Year Artifact which is caused by the annual observing schedule of the MACHO project, that the star is outside the boundaries of any period-luminosity classification, or that Fraser et al. (2008, Cat. J/AJ/136/1242) were unable to classify this object. The other abbreviations used to characterise the variability of the different objects are Population II Cepheids (Ceph.) which include the subclass of RV Tauri stars (RVT), semi-regular variables (SRV) with the subclass of sequence-D variables (Seq. D) that were recognized by us, objects with lightcurves in Fig. 18 that show long-term, slow variations (SV), RCrB stars (RCrB), objects in regions of very strong nebular emission (em), Ae and Be stars (AB) and objects that do not show strong evidence of variability (NV). For all Population II Cepheids, the periods we computed between deep minima or two cycles of the light curve if the minima are of equal depth, are listed in days.
Acknowledgements: Els van Aarle, els.vanaarle(at)
(End) Els van Aarle [K.U.Leuven], Patricia Vannier [CDS] 11-Apr-2011
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