Mapping low-latitude stellar substructure with SEGUE photometry

被引：0

作者：

de Jong, Jelte T. A. ^{[1
]}

Yanny, Brian ^{[2
]}

Rix, Hans-Walter ^{[1
]}

Bell, Eric F. ^{[1
]}

Dolphin, Andrew E. ^{[3
]}

机构：

[1] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[2] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA

[3] Raytheon Corp, Waltham, MA 02451 USA

来源：

GALAXY DISK IN COSMOLOGICAL CONTEXT, PROCEEDINGS OF THE 254TH SYMPOSIUM OF THE IAU | 2009年 / 254期

基金：

美国国家航空航天局; 美国国家科学基金会;

关键词：

Galaxy: stellar content; Galaxy: structure; DIGITAL SKY SURVEY; CANIS-MAJOR OVERDENSITY; MILKY-WAY; DWARF GALAXY; DENSITY; STARS; ACCRETION; ORIGIN; MAPS; SDSS;

D O I：

10.1017/S1743921308027488

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Encircling the Milky Way at low latitudes, the Low Latitude Stream is a large stellar structure, the origin of which is as yet unknown. As part of the SEGUE survey, several photometric scans have been obtained that cross the Galactic plane, spread over a longitude range of 50 degrees to 203 degrees. These data allow a systematic study of the structure of the Galaxy at low latitudes, where the Low Latitude Stream resides. We apply color-magnitude diagram fitting techniques to map the stellar (sub)structure in these regions, enabling the detection of overdensities with respect to smooth models. These detections can be used to distinguish between different models of the Low Latitude Stream, and help to shed light on the nature of the system.

引用

页码：121 / +

页数：2

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