Quantitative spectral classification of galactic disc K-M stars from sectrophotometric measurements

Malyuto, V.; Oestreicher, M. O.; Schmidt-Kaler, Th.

doi:10.1093/mnras/286.2.500

Cited by 23 publications

(20 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Since the publication of Paper II some modifications have been made to the stellar library. For example, HD 283916 is classified as a K2III (Malyuto et al 1997) instead of a K5V star as quoted by Silva & Cornell (1992). We have checked that when we run the synthesis programme without this star, the solutions imply a stronger contribution from giants.…”

Section: Methodsmentioning

confidence: 83%

Stellar populations in Active Galactic Nuclei III

Boisson¹,

Joly²,

Pelat³

et al. 2004

A&A

View full text Add to dashboard Cite

Abstract. In this paper we apply the stellar population synthesis method previously described in Boisson et al. (2000) to five more AGN. The analysis of these new data strengthen our previous conclusions: i) homogeneity of the stellar population within a class of nuclear activity regardless of the morphological type of the host galaxy; ii) populations within the nuclear regions of LINERs and Seyfert 2s are different: LINERs have a very old metal-rich population while in the Seyfert 2s a contribution of a weak burst of star formation is observed together with the old high metallicity component; iii) in the circum-nuclar region (200 pc ≤ D ≤ 1 kpc) of all the active galaxies in our sample, except for NGC 2992, we detect an old burst of star formation (0.2−1 Gyr),which is contrary to what is observed in normal galaxies. We note that the broad OIλ8446 Å emission line detected in the spectrum of the nucleus of NGC 2992 confirms its classification as a Seyfert 1.

show abstract

Section: Methodsmentioning

confidence: 83%

Stellar populations in Active Galactic Nuclei III

Boisson¹,

Joly²,

Pelat³

et al. 2004

A&A

View full text Add to dashboard Cite

show abstract

“…This results in a spectral class of M 4-M 5. The scheme of TiO indices (Malyuto et al 1997) (7878) TiO (8432) TiO (6322) TiO (7666) TiO (7053) TiO (6159) TiO (5597) TiO (5448) of the TiO to the NaD and Mgb indices propose luminosity class III. The most reliable classification is the direct comparison with standards, using the identical instrument setup.…”

Section: Spectroscopymentioning

confidence: 99%

Optical spectroscopy of IRAS 02091+6333

Kimeswenger

Bacher

Emprechtinger

et al. 2003

A&A

View full text Add to dashboard Cite

Abstract. We present a detailed spectroscopic investigation, spanning four winters, of the asymptotic giant branch (AGB) star IRAS 02091+6333. Zijlstra & Weinberger (2002) found a giant wall of dust around this star and modelled this unique phenomenon. However their work suffered from the quality of the optical investigations of the central object. Our spectroscopic investigation allowed us to define the spectral type and the interstellar foreground extinction more precisely. Accurate multi band photometry was carried out. This provides us with the possibility to derive the physical parameters of the system. The measurements presented here suggest a weak irregular photometric variability of the target, while there is no evidence of a spectroscopic variability over the last four years.

show abstract

“…In the ILC -ISTdiagram (see Fig. 9 in Malyuto et al (1997)) M dwarfs, giants and supergiants are clearly separated. Nevertheless one cannot directly measure luminosities with it as ILC: is strongly dependent on temperature also.…”

Section: Introductionmentioning

confidence: 97%

“…Nothing has been told, however, about their luminosities and distances. To do this, we develop a further step in the new classification system for M stars introduced by Malyuto et al (1997) who have shown that indices measuring the strength of absorption features allow an accurate and homogeneous classification. As temperature criterion a spectral index IST measuring the features NaD + TiOyi, Ti076 and TiOyL, + TiOyl has been introduced, while as luminosity criterion a luminosity index ILC measuring the features FeI + TiOal and Mgb + TiOao has been defined.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The luminosity index for M stars and the distance to the LMC

Schmidt-Kaler¹,

Oestreicher²

1998

Astron Nachr

Self Cite

View full text Add to dashboard Cite

On the bases ofthe new classification system introduced by Malyuto et al. (1997) a new technique to determine luminosities for M type stars has been established. Due to the lack of accurate distances and their inhomogeneity especially for supergiants the intrinsic scatter is rather high with 0.4 to 0.5 mag. The uncertainty of the zeropoint is 0.07 to 0.08 mag. Applying our new method to M supergiant members of the LMC a distance modulus of 18.34 & 0.09 mag is derived which agrees well with recent work. The luminosities of the stars range from those of galactic Iab to those of Ia-Ia-0 supergiants, i.e. the upper luminosity limit does not exceed that of their galactic counterparts. Like the CaII H and K emission technique of Wilson & Bappu (1957), for which a revised calibration is given, the new method spans an extremely wide range of luminosities. It is less universal, as it can be applied to M stars only, but not to K stars. On the other hand the Wilson-Bappu-method requires high resolution spectroscopy so that it is restricted to bright stars in our Galaxy. Our new technique may be applied to faint stars in nearby galaxies since it requires low resolution spectroscopy only.

show abstract

Quantitative spectral classification of galactic disc K-M stars from sectrophotometric measurements

Cited by 23 publications

References 0 publications

Stellar populations in Active Galactic Nuclei III

Stellar populations in Active Galactic Nuclei III

Optical spectroscopy of IRAS 02091+6333

The luminosity index for M stars and the distance to the LMC

Contact Info

Product

Resources

About