研究目的
To analyze UVIT observations of the central part of the bulge of M31 to detect the hottest stars and understand the star formation rate in the bulge of M31.
研究成果
The study detected hot main-sequence stars in the bulge of M31, indicating a low but significant rate of star formation in the very recent past. This provides new insights into the stellar populations and star formation history of M31's bulge.
研究不足
The study is limited by the spatial resolution of UVIT and the crowding of cool stars in the M31 bulge, which may bias the cool star fit parameters. The photometry's completeness in the bright central part of the bulge is uncertain, affecting the star formation rate estimation.
1：Experimental Design and Method Selection:
The study utilized the ASTROSAT Observatory's UVIT instrument for UV observations of M31's bulge. The methodology involved cross-matching UVIT sources with PHAT catalog sources to obtain multi-band SEDs and fitting these SEDs with stellar models.
2：Sample Selection and Data Sources:
The sample consisted of UVIT observations of the central 7′ part of M31's bulge. Data sources included UVIT observations and the PHAT catalog from HST.
3：List of Experimental Equipment and Materials:
The primary instrument used was the UVIT aboard ASTROSAT, with filters covering 120–280 nm. The study also referenced data from the PHAT survey conducted with HST's Wide Field Camera 3 and Advanced Camera for Surveys.
4：Experimental Procedures and Operational Workflow:
The workflow involved identifying UVIT sources, cross-matching with PHAT sources, performing photometry, and fitting SEDs with stellar models to derive physical parameters of the stars.
5：Data Analysis Methods:
Data analysis included photometry of UVIT sources, cross-matching with PHAT sources, and SED fitting using Castelli and Kurucz stellar models to derive star parameters.
独家科研数据包，助您复现前沿成果，加速创新突破
获取完整内容
