J/A+AS/117/227 Dwarf effective temperatures (Alonso+ 1996) ================================================================================ Determination of effective temperatures for an extended sample of dwarfs and subdwarfs (F0-K5). Alonso A., Arribas S., Martinez-Roger C. =1996A&AS..117..227A ================================================================================ ADC_Keywords: Stars, subdwarf ; Effective temperatures ; Photometry, infrared Keywords: stars: fundamental parameters - stars: Population II - stars: subdwarfs - stars: general Description: We have applied the InfraRed Flux Method (IRFM) to a sample of 475 dwarfs and subdwarfs in order to derive their effective temperatures with a mean accuracy of about 1.5%. We have used the new homogeneous grid of theoretical model atmosphere flux distributions developed by Kurucz (1991, 1993) for the application of the IRFM. The atmospheric parameters of the stars cover, roughly, the ranges: 3500K<=T_eff_<=8000K; -3.5<=[Fe/H]<=+0.5; 3.5<=log(g)<=5. The monochromatic infrared fluxes at the continuum, and the bolometric fluxes are derived using recent results, which satisfy the accuracy requirements of the work. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table4.dat 134 462 Effective temperatures table4a.tex 312 457 LaTeX version of table4, part 1 table4b.tex 167 285 LaTeX version of table4, part 2 -------------------------------------------------------------------------------- See also: J/A+AS/107/365 : Dwarfs and subdwarfs IR photometry (Alonso+, 1994) J/A+AS/131/209 : Giants JHK(L') photometry (Alonso+ 1998) Byte-by-byte Description of file: table4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 12 A12 --- ID Identification (1) 14 A1 --- n_ID Individual note on ID (2) 17- 20 F4.2 [cm/s2] logg Surface gravity 22- 26 F5.2 [Sun] [Fe/H] Metallicity 28- 36 E9.3 mW/m2 FBol Bolometric flux (erg/cm2/s) 38- 41 F4.2 mag E(B-V) Interestellar redenning 43- 51 E9.3 dW/m2/nm FJ ? Monochromatic flux in the band J (6) 53- 57 F5.3 --- qJ ? q-factor in the band J (7) 59 A1 --- l_TJ limit flag on TJ 60- 63 I4 K TJ ? Effective temperature derived in the band J 64 A1 --- n_TJ [])] Note on TJ (3) 66- 68 I3 K e_TJ ? rms uncertainty on TJ (4) 70- 78 E9.3 dW/m2/nm FH ? Monochromatic flux in the band H (6) 80- 84 F5.3 --- qH ? q-factor in the band H (7) 86 A1 --- l_TH Limit flag on TH 87- 90 I4 K TH ? Effective temperature derived in the band H 91 A1 --- n_TH []] Note on TH (3) 93- 95 I3 K e_TH ? rms uncertainty on TH (4) 97-105 E9.3 dW/m2/nm FK ? Monochromatic flux in the band K (6) 107-111 F5.3 --- qK ? q-factor in the band K (7) 114-117 I4 K TK ? Effective temperature derived in the band K 119-121 I3 K e_TK ? rms uncertainty on TK (4) 125-128 I4 K Tmean ? Weighted effective temperature derived from TJ, TH and TK 129 A1 --- n_Tmean [)] Note on Tmean (3) 131-133 I3 K e_Tmean ? rms uncertainty on Tmean (5) -------------------------------------------------------------------------------- Note (1): Giclas number has been preferred when available. HD, BD, HR and GJ numbers were used otherwise. The stars are ordered in right ascension Note (2): Notes are numbered as follows: 1 = SB501: Wrong FJ, (J=11.22). 2 = G036-050: The error in FJ is greater than 10%, hence no TJ is provided. 3 = G178-030: Very faint star, J=11.63, H=11.31 and K=11.127. 4 = G167-011: The error in FJ is greater than 20%. The faintest star of the sample (J=12.99). 5 = HR6228: Wrong FJ. 6 = G017-037: Very faint star, J=11.706, H=11.300 and K=11.297. 7 = G021-006: Wrong FJ, (J=10.38). 8 = G126-063: Faint star, J=10.69, H=10.64 and K=10.59. 9 = G217-008: Wrong FJ. Note (3): -- A bracket indicates that the temperature has not been considered in the mean as explained in Sect. 5. -- A parentheses indicates temperatures under 4000 K. In this case there isn't estimation of the total error because of the uncertainties of the model fluxes in this range. Note (4): Error computed considering errors in FBol, FJ, logg and [Fe/H]. Note (5): Mean error computed considering linear transmission of errors from e_TJ, e_TH and e_TK. Note (6): in 10^2^ erg.cm^-2^.s^-1^.nm^-1^ Note (7): the q factor is the ratio between the monochromatic and integrated fluxes (it corrects the effects of the different curvatures in the flux density distribution). It is a function of the stellar parameters (T, g, metallicity) and wavelength. -------------------------------------------------------------------------------- Courtesy: Angel Alonso ================================================================================ (End) Patricia Bauer [CDS] 18-Jan-1996