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Home All issues Volume 498 / No 1 (April IV 2009) A&A, 498 1 (2009) 127-138 Full HTML
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Table 1:

Object designations and general characteristics. Star with their names printed in italic have luminosities which also allow an AGB star identification. The bolometric magnitudes were computed from the dereddened K band magnitudes, using the bolometric corrections of Levesque et al. (2005).

Source		 ISO TDT Spectral Variabilitya Perioda Kraemerb Distancec $A_{\rm {V}}$d $M_{\rm bol}$
  number type type [d] class [pc]    
HD 14242 61 301 202 M2Iab Lc   2.SEa: 2290 1.63 -6.93
AD PER 78 800 921 M2.5Iab SRc 363 2.SEa: 2290 1.63 -7.42
HD 14404 45 501 704 M1Iab Lc   2.SEap: 2290 1.63 -7.23
SU PER 43 306 303 M3Iab SRc 533 2.SEc 2290 1.63 -7.90
RS PER 45 501 805 M4Iab SRc 245 2.SEc 2290 1.63 -7.74
S PER 42 500 605 M4.5Iab SRc 822 3.SE 2290 1.63 -8.18
HD 14580 42 701 401 M1Iab Lc   1.NO: 2290 1.63 -6.49
HD 14826 61 601 203 M2Iab Lc   2.SEa: 2290 1.63 -7.36
YZ PER 47 301 604 M2Iab SRb 378 2.SEc 2290 1.63 -7.50
W PER 63 702 662 M4.5Iab SRc 485 2.SEc 2290 1.63 -7.74
$\rho$ PER 79 501 105 M4II SRb 50 1.NO 100 0.82 -4.20
HR 1939 86 603 434 M2Iab Lc   2.SEa 420 0.66 -4.51
$\alpha $ ORI 69 201 980 M2Iab SRc 2335 2.SEcp 131 0.09 -7.19
HD 90586 25 400 410 M2Iab/Ib     2.SEc 641 0.40 -4.76
R CEN 07 903 010 M5IIevar M 546 2.SEap 641 0.95 -6.94
$\alpha $ SCO 08 200 369 M1.5Iabb Lc   2.SEcp 185 0.72 -7.86
$\alpha $ HER 28 101 115 M5Iab SRc   1.NOp 117 0.42 -5.99
$\sigma $ OPH 10 200 835 K3Iab     1.NO 360 0.68 -4.33
HR 7475 31 601 515 K4Ib N:   1.NO 704 0.91 -5.87
NR VUL 53 701 751 K3Iab Lc   2.SEc 2000 2.98 -8.01
BD+35 4077 73 000 622 M2.5Iab Lc   2.SEb 1820 2.61 -7.48
RW CYG 12 701 432 M3Iab SRc 550 2.SEc 1200 3.54 -7.77
IRC +40427 53 000 406 M1:Iab     2.SEap: 2000 1.79 -6.89
$\mu $ CEP 08 001 274 M2Ia SRc 730 2.SEc 830 1.84 -8.86
V354 CEP 41 300 101 M2.5Iab Lc   2.SEc 3500 2.00 -8.51
U LAC 41 400 406 M4Iab:e SRc   2.SEc 3470 1.74 -8.30
PZ CAS 09 502 846 M3Iab SRc 925 2.SEc 2510 2.11 -8.89
a Combined General Catalogue of Variable Stars (Kholopov et al. 1998); b Kraemer et al. (2002); c distances below 1 kpc come from parallax measurements with HIPPARCOS (Perryman et al. 1997). Distances equal to 2 kpc are actually unknown and distances greater than 1 kpc are cluster distances from Humphreys (1978). $\mu $ Cep is an exception: we use the distance of Humphreys (1978) instead of the poor parallax measurement; d ISM extinction estimates for stars within 1 kpc come from the galactic model of Arenou et al. (1992). All other stars and $\mu $ Cep have estimates based on the extinction toward early-type stars in the corresponding clusters.

Source LaTeX | All tables | In the text

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