J/ApJ/754/35 Red supergiant stars in the SMC. II. (Yang+, 2012)
The period-luminosity relation of red supergiant stars in the Small Magellanic Cloud. Yang M., Jiang B.W. <Astrophys. J., 754, 35 (2012)> =2012ApJ...754...35Y 2012ApJ...754...35Y
ADC_Keywords: Magellanic Clouds ; Stars, late-type ; Stars, supergiant ; Stars, variable ; Photometry, infrared Keywords: galaxies: individual: SMC; stars: oscillations; stars: variables: general; supergiants Abstract: The characteristics of light variation of red supergiant (RSG) stars in the Small Magellanic Cloud (SMC) are analyzed based on the nearly 8-10 year data collected by the ASAS and MACHO projects. The 126 identified RSGs are classified into five categories accordingly: 20 with poor photometry, 55 with no reliable period, 6 with semi-regular variation, 15 with a long secondary period (LSP) and distinguishable short period, and 30 with only an LSP. For the semi-regular variables and the LSP variables with distinguishable short period, the KS-band period-luminosity (P-L) relation is analyzed and compared with that of the Galaxy, the Large Magellanic Cloud, and M33. It is found that the RSGs in these galaxies obey a similar P-L relation except for those in the Galaxy. In addition, the P-L relations in the infrared bands, namely, the 2MASS JHKS, Spitzer/IRAC, and Spitzer/MIPS 24 µm bands, are derived with high reliability. The best P-L relation occurs in the Spitzer/IRAC [3.6] and [4.5] bands. Based on the comparison with the theoretical calculation of the P-L relation, the mode of pulsation of RSGs in the SMC is suggested to be the first-overtone radial mode. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table1.dat 127 140 Infrared catalog of the 140 SMC red supergiant candidates (RSGs) table3.dat 64 21 Results of time-series analysis by PDM, Period04, and CLEAN methods for 6 semi-regular and 15 LSP RSGs with short periods table6.dat 32 31 Period of long secondary period (LSP) of 31 SMC RSG s obtained by PDM, Period04, and CLEAN methods -------------------------------------------------------------------------------- See also: II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) II/305 : SAGE LMC and SMC IRAC Source Catalog (IPAC 2009) II/236 : UBVR CCD survey of the Magellanic clouds (Massey+, 2002) II/264 : ASAS Variable Stars in Southern hemisphere (Pojmanski+, 2002-2005) II/247 : Variable Stars in the Large Magellanic Clouds (MACHO, 2001) J/ApJ/727/53 : Red supergiant stars in the LMC. Paper I. (Yang+, 2011) J/AJ/139/1168 : CaII spectroscopy of SMC fields stars (Parisi+, 2010) J/AJ/138/517 : CaII spectroscopy of SMC red giants (Parisi+, 2009) J/AJ/136/1039 : CaII index of SMC red giant branch stars (Carrera+, 2008) J/AJ/132/1630 : CaII spectro. in Magellanic Cloud clusters (Grocholski+, 2006) J/AJ/131/2514 : Radial velocities of red giants in the SMC (Harris+, 2006) J/A+A/425/595 : OGLE+2MASS+DENIS LPV in Magellanic Clouds (Groenewegen, 2004) J/AJ/126/2867 : Red supergiants in Magellanic Clouds (Massey+, 2003) J/ApJ/501/153 : VRB photometry of red supergiants (Massey 1998) J/A+A/304/347 : 40 field red supergiants in the SMC (Meliani+, 1995) Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- Seq [1/140] Running sequence number 5- 29 A25 --- Name Source name 31- 32 I2 h RAh Hour of right ascension (J2000) 34- 35 I2 min RAm Minute of right ascension (J2000) 37- 41 F5.2 s RAs Second of right ascension (J2000) 43 A1 --- DE- Sign of declination (J2000) 44- 45 I2 deg DEd Degree of declination (J2000) 47- 48 I2 arcmin DEm Arcminute of declination (J2000) 50- 53 F4.1 arcsec DEs Arcsecond of declination (J2000) 55- 60 F6.3 mag Jmag [8.3/12.7]? 2MASS J-band magnitude 62- 67 F6.3 mag Hmag [7.6/11.9]? 2MASS H-band magnitude 69- 74 F6.3 mag Ksmag [7.4/11.6]? 2MASS Ks-band magnitude 76- 81 F6.3 mag [3.6] [6.6/11]? Spitzer/IRAC 3.6um magnitude 83- 88 F6.3 mag [4.5] [6.3/10.8]? Spitzer/IRAC 4.5um magnitude 90- 95 F6.3 mag [5.8] [5.5/10.6]? Spitzer/IRAC 5.8um magnitude 97-102 F6.3 mag [8.0] [4.7/10.4]? Spitzer/IRAC 8um magnitude 104-109 F6.3 mag [24] [2.5/10.1]? Spitzer/MIPS 24um magnitude 111-117 A7 --- SpT MK spectral type (1) 119-123 A5 --- Ref Reference (2) 125-127 A3 --- Src Photometry data resource (3) -------------------------------------------------------------------------------- Note (1): Spectral types are from Massey & Olsen (2003, Cat. J/AJ/126/2867) and Levesque et al. (2006ApJ...645.1102L 2006ApJ...645.1102L, 2007ApJ...667..202L 2007ApJ...667..202L) and all have been updated. Note (2): Reference as follows: CF81 = Catchpole & Feast 1981MNRAS.197..385C 1981MNRAS.197..385C; WBF83 = Wood et al. 1983ApJ...272...99W 1983ApJ...272...99W; M03 = Massey & Olsen 2003, Cat. J/AJ/126/2867; L06 = Levesque et al. 2006ApJ...645.1102L 2006ApJ...645.1102L; V08 = van Loon et al. 2008A&A...487.1055V 2008A&A...487.1055V; V10 = van Loon et al. 2010AJ....139.1553V 2010AJ....139.1553V Note (3): The photometric data in visual bands are taken from the following databases: A = ASAS (Pojmanski 2002, Cat. II/264) M = MACHO (Alcock et al. 1997ApJ...486..697A 1997ApJ...486..697A) -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- Seq [5/140] Sequential number 5- 9 F5.2 mag <Vmag> [11.9/13.2] Mean V-band magnitude 11- 15 F5.2 mag Mbol [-8.8/-7.8]? Bolometric absolute magnitude 17- 19 I3 d Per [195/728] Period derived from PDM method (G1) 21- 24 F4.2 mag Vamp [0.1/0.5] V-band amplitude from PDM 26- 29 F4.2 --- Theta [0.1/0.7] Θ value from PDM (ratio of the bin to total variance) 31- 33 I3 d Per04 [195/728] Period from Period04 method (G1) 35- 38 F4.2 mag Vamp04 [0.04/0.5] V-band amplitude from Period04 40- 43 F4.2 --- Phase [0/1] Phase from Period04 45- 47 I3 d CLEAN [195/766] Period from CLEAN method (G1) 49- 51 I3 d[195/740] Average period from CLEAN 53- 54 I2 d e_
[0/22]
uncertainty from CLEAN 56- 58 I3 --- Np [175/214] Number of points from CLEAN method 60 A1 --- Type [SL] Variable type (1) 62- 64 A3 --- Ref Reference (2) -------------------------------------------------------------------------------- Note (1): Variable type as follows: S = semi-regular RSGs; L = LSP RSGs with distinguishable short periods. Note (2): Reference for Mbol as follows: L06 = Levesque et al. 2006ApJ...645.1102L 2006ApJ...645.1102L L07 = Levesque et al. 2007ApJ...667..202L 2007ApJ...667..202L L09 = Levesque et al. 2009ASPC..412...33L 2009ASPC..412...33L -------------------------------------------------------------------------------- Byte-by-byte Description of file: table6.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- Seq [5/129] Sequential number 5- 8 F4.2 mag Amp [0.02/0.4] Amplitude 10- 13 I4 d PDM [1154/2749] Period derived from PDM (G1) 15- 18 I4 d Per04 [1209/2656] Period from Period04 (G1) 20- 23 I4 d CLEAN [1184/2633] Period derived from the CLEAN method (G1) 25- 28 I4 d
[1182/2650] Mean long secondary period (LSP) 30- 32 I3 d e_ [10/151] uncertainty -------------------------------------------------------------------------------- Global note: Note (G1): Methods are: PDM = Phase Dispersion Minimization method (Stellingwerf, 1978ApJ...224..953S 1978ApJ...224..953S). PDM2 (Yang and Jiang 2011, J/ApJ/727/53) was used instead of the original version used in Paper I Period04 = method of deriving the period of light variation from Lenz (2004CoAst.144...41L 2004CoAst.144...41L). CLEAN = method which deconvolves the spectral window function from the "dirty" Discrete Fourier Transform (DFT) spectrum by using a one-dimensional version of the iterative CLEAN algorithm (Hoegbom, 1974A&AS...15..417H 1974A&AS...15..417H). See section 2.2 for details. -------------------------------------------------------------------------------- History: From electronic version of the journal Reference: Yang & Jiang Paper I. 2011ApJ...727...53Y 2011ApJ...727...53Y Cat. J/ApJ/727/53
(End) Emmanuelle Perret [CDS] 27-Feb-2014
| 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 |