Abstract
Abstract In this paper, we present an online multiwavelength database of water masers in star-forming regions of the Galaxy. The collected data represent ∼95% of all observations of water masers in star-forming regions published since 1989. Nineteen transitions are included, from 22 GHz to 1.88 THz. The MaserDB.net information system provides fast and open access to the collected data, including maser tabular data, spectra, and interferometric maser spot data. The database covers ∼18,700 individual observations and ∼7200 maser detections. The data on the water maser detection are available for ∼2600 sources, and interferometric data are available for ∼560 sources. Statistical analysis of the water masers’ data and comparison with other abundant maser species found in star-forming regions (OH and CH3OH of class I and II) show that water masers are the most ubiquitous maser type. Access to the water maser database is available online at https://MaserDB.net. The database can be queried using a web search form or Structured Query Language.
Highlights
Water maser emission is a unique phenomenon of interstellar matter, which is currently mainly found in star formation regions (SFRs), evolved stars, and circumnuclear regions of supermassive black holes in external galaxies
It was shown in Furuya et al (2003) that water masers are primarily related to young stellar objects (YSOs) of class 0 and sometimes class I, but no water masers are found to be associated with class II YSOs
We present a database of water masers in galactic star-forming regions with the following characteristics: 1. Data are collected from the available literature and completed at a level of 95% for observations of SFR published since 1989
Summary
Water maser emission is a unique phenomenon of interstellar matter, which is currently mainly found in star formation regions (SFRs), evolved stars, and circumnuclear regions of supermassive black holes in external galaxies. Unlike the 6.7 GHz methanol masers, which are considered to be associated exclusively with the formation of massive stars, water masers are associated with low-mass stellar objects. It was shown in Furuya et al (2003) that water masers are primarily related to young stellar objects (YSOs) of class 0 and sometimes class I, but no water masers are found to be associated with class II YSOs. Certain conditions are necessary for water maser formation— high temperature and density (Elitzur et al 1989; Yates et al 1997; Gray et al 2016).
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