Ices in star-forming regions: Highlights from ISO, laboratory and theory

被引：0

作者：

Ehrenfreund, P ^{[1
]}

Boogert, ACA ^{[1
]}

Gerakines, PA ^{[1
]}

Schutte, WA ^{[1
]}

Thi, WF ^{[1
]}

Tielens, AGGM ^{[1
]}

VandenBussche, B ^{[1
]}

van Dishoeck, EF ^{[1
]}

Whittet, DCB ^{[1
]}

机构：

[1] Leiden Observ, NL-2300 RA Leiden, Netherlands

来源：

FIRST ISO WORKSHOP ON ANALYTICAL SPECTROSCOPY: WITH SWS, LWS, PHT-S, AND CAM-CVF | 1997年 / 419卷

关键词：

ISM; molecules; dust; stars; pre-main sequence; comets; volatiles;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present ISO observations of bright star-forming regions, obtained with the Short Wavelength Spectrometer (SWS). ISO allows us to study for the first time the complete inventory of interstellar ices. First results showed the ubiquitous presence of abundant: CO2 ice in space and provided new insights into the gas to solid ratio of many interstellar molecules. According to their evolutionary state, young objects show interstellar ice features such as H2O, CO, CO2, CH4 (and other minor species), as well as interstellar gas features, such as H2O, CO and CO2. The more evolved objects are dominated by strong atomic emission lines and polycyclic aromatic hydrocarbons (PAHs): ISO spectra of interstellar gas and dust in comparison with laboratory results and theoretical models constrain gas/grain interactions, temperature and irradiation conditions towards star-forming regions, and consequently their evolution. Well established abundances of interstellar molecules will also guide the interpretation of past and future cometary observations. Recent and future ISO results thus allow to study the connection between interstellar and cometary dust and consequently provide constraints on the formation of the Solar System.

引用

页码：3 / 9

页数：7