Faint M dwarfs and the structure of the galactic disk

被引：27

作者：

Reid, IN ^{[1
]}

Gizis, JE ^{[1
]}

Cohen, JG ^{[1
]}

Pahre, MA ^{[1
]}

Hogg, DW ^{[1
]}

Cowie, L ^{[1
]}

Hu, E ^{[1
]}

Songaila, A ^{[1
]}

机构：

[1] UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC | 1997年 / 109卷 / 735期

基金：

美国国家科学基金会;

关键词：

D O I：

10.1086/133914

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We use broadband photometry and low-resolution spectra of a complete sample of late-type K and M dwarfs brighter than I=22 in three fields at high galactic latitude to study issues relating to galactic structure and large-scale abundance gradients in the Galaxy. The observed starcounts in each field are a good match to the predictions of models based on deep starcount data in other intermediate-latitude fields, and these models identify the late-type stars as members of the Galactic disk. Abundances for these late-type stars are estimated via narrow-band indices that measure the strength of the TiO and CaH bands in their spectra. Our results show that the average abundance in the Galactic disk remains close to solar even at heights of more than 2 kpc above the Plane.

引用

页码：559 / 565

页数：7

共 25 条

[1] MODEL ATMOSPHERES FOR M (SUB)DWARF STARS .1. THE BASE MODEL GRID [J].