Resumen
Stars brighter than the RGB tip of an old-globular cluster like population are seen in (he M 31 and M 33 bulges from HST (Rich & Mighell 1995), and ground based IR observations (Rich et al. 1993, Minniti et al. 1994). We present radial velocities for individual giants selected among stars in the bright plume of relatively young stars seen in our IR color-magnitude diagrams of the M 33 bulge. The mean velocity of our sample is V = -182 ±13, and the velocity dispersion is σ= 34 ± 9 km/s. Based on the mean velocity we conclude that all but one of these stars are members of M 33. Based on the velocity dispersion, these stars are either associated with the M 33 disk or with the M 33 bulge.
| Idioma original | English |
|---|---|
| Páginas (desde-hasta) | 715-720 |
| Número de páginas | 6 |
| Publicación | Astronomy and Astrophysics |
| Volumen | 306 |
| N.º | 3 |
| Estado | Published - 20 feb 1996 |
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ASJC Scopus subject areas
- Space and Planetary Science
- Astronomy and Astrophysics
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Velocities of supergiants in the bulge of M 33. / Minniti, Dante.
En: Astronomy and Astrophysics, Vol. 306, N.º 3, 20.02.1996, p. 715-720.Resultado de la investigación: Article
TY - JOUR
T1 - Velocities of supergiants in the bulge of M 33
AU - Minniti, Dante
PY - 1996/2/20
Y1 - 1996/2/20
N2 - Stars brighter than the RGB tip of an old-globular cluster like population are seen in (he M 31 and M 33 bulges from HST (Rich & Mighell 1995), and ground based IR observations (Rich et al. 1993, Minniti et al. 1994). We present radial velocities for individual giants selected among stars in the bright plume of relatively young stars seen in our IR color-magnitude diagrams of the M 33 bulge. The mean velocity of our sample is V = -182 ±13, and the velocity dispersion is σ= 34 ± 9 km/s. Based on the mean velocity we conclude that all but one of these stars are members of M 33. Based on the velocity dispersion, these stars are either associated with the M 33 disk or with the M 33 bulge.
AB - Stars brighter than the RGB tip of an old-globular cluster like population are seen in (he M 31 and M 33 bulges from HST (Rich & Mighell 1995), and ground based IR observations (Rich et al. 1993, Minniti et al. 1994). We present radial velocities for individual giants selected among stars in the bright plume of relatively young stars seen in our IR color-magnitude diagrams of the M 33 bulge. The mean velocity of our sample is V = -182 ±13, and the velocity dispersion is σ= 34 ± 9 km/s. Based on the mean velocity we conclude that all but one of these stars are members of M 33. Based on the velocity dispersion, these stars are either associated with the M 33 disk or with the M 33 bulge.
KW - Galaxies: individual: M 33
KW - Galaxies: kinematics and dynamics
KW - Galaxies: structure; stellar content
UR - http://www.scopus.com/inward/record.url?scp=0001200933&partnerID=8YFLogxK
M3 - Article
AN - SCOPUS:0001200933
VL - 306
SP - 715
EP - 720
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
IS - 3
ER -