M-Type Stars in NGC 7419.

Blanco, V. M.; Nassau, J. J.; Stock, J.; Wehlau, W. H.

doi:10.1086/146029

Cited by 13 publications

(17 citation statements)

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“…An anomalous amount of supergiants (six) has been noticed in this cluster [13]. Five members of the cluster are stars of spectral class later than M2.5 and one is a carbon star.…”

Section: General Characteristics Of the Cluster Ngc 7419mentioning

confidence: 73%

B and Be-stars in the young open stellar clusters NGC 659 and NGC 7419

Malchenko

Tarasov

2011

Astrophysics

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The populations of B and Be-stars in the young open clusters NGC 7419 and NGC 659 are studied. Lowresolution spectral observations in the region of the Hα line are used to study 34 members of NGC 7419 and additional spectra in the range λ3700-6200 Å are obtained for 12 stars. During the period of our observations, four previously identified Be-stars manifested an absorption profile for the Hα line. Emission in the Hα line is observed in the spectra of 21 objects. The members of the cluster NGC 7419 are classified as to spectral type. The position of the Be-stars on a two-color IR diagram and a comparison with the position of the objects in other clusters with similar ages cast doubt on the existence of two starformation waves. Moderate resolution spectra were obtained for 22 stars in the cluster NGC 659 over wavelengths of λ4050-5200 Å and for 7 objects in the neighborhood of the Hα line. Emission is observed in both the Hα and Hβ lines for two of the five Be-stars that were studied, while faint emission appears only in the Hα line in one of the stars. The other members of the cluster show no signs of emission in these spectra. T eff , log g, and Vsini are estimated for the observed stars. It is found that 5 of the objects are not members of the cluster.

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“…An anomalous amount of supergiants (six) has been noticed in this cluster [13]. Five members of the cluster are stars of spectral class later than M2.5 and one is a carbon star.…”

Section: General Characteristics Of the Cluster Ngc 7419mentioning

confidence: 73%

B and Be-stars in the young open stellar clusters NGC 659 and NGC 7419

Malchenko

Tarasov

2011

Astrophysics

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“…4 is used for distinguishing some of the non-members. All stars which were detected both in the R C and I C -filter frames are shown in Fig Bhatt et al (1993) number, E precedes the number of a star in the eastern region of the cluster, W, a star in the western region, (3): Kohoutek & Wehmeyer (1997) number, (4) and (5) (Blanco et al 1955;Fawley & Cohen 1974;Beauchamp et al 1994, henceforth B94). The coolest of them is MY Cephei = IRAS 22525+6033, an Lb or SRc-type variable of spectral type M7.5 I, known also to be an H 2 O maser (Dickinson et al 1978) and an OH/IR source (Alcolea et al 1990).…”

Section: Observations and Reductionsmentioning

confidence: 99%

NGC 7419: An open cluster rich in Be stars

Pigulski¹,

Kopacki²

2000

Astron. Astrophys. Suppl. Ser.

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Abstract. The results of our CCD photometric Hα observations of NGC 7419 are presented. The observations resulted in a discovery of 17 new Be stars and two other emission-line objects. In consequence, the number of known Be stars in this young cluster increased more than twofold and equals now to 31. This is at present the largest number of Be stars known in any galactic open cluster. Moreover, we estimate that these 31 Be stars constitute 36 ± 7% of all cluster B-type stars brighter than R C = 16.1 mag. This locates NGC 7419 among these open clusters which are richest in Be stars such as galactic NGC 663, NGC 330 in SMC, and NGC 1818A in LMC.

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“…Blanco et al (1955) have reported the distance of this cluster as ∼6 kpc based on the RI photometric observations. A similar value for cluster distance has also been obtained by Moffat & Vogt (1973).…”

Section: Introductionmentioning

confidence: 99%

“…Deep optical UBVRI observations (V ∼ 22.0 mag), narrow-band Hα photometric observations along with the Two Micron All Sky Survey (2MASS), Infrared All Sky Survey (IRAS), Midcourse Space Experiment (MSX) and XMM-Newton archival data are used to understand the X-ray emission properties of Herbig Ae/Be stars, and the global scenario of star formation in the cluster NGC 7419 and its surrounding region. Blanco et al (1955) have reported the distance of this cluster as ∼6 kpc based on the RI photometric observations. A similar value for cluster distance has also been obtained by Moffat & Vogt (1973).…”

Section: Introductionmentioning

confidence: 99%