A global view on star formation: The GLOSTAR Galactic plane survey

Nguyen, H.; Rugel, M.; Murugeshan, C.; Menten, K. M.; Brunthaler, A.; Urquhart, J. S.; Dokara, R.; Dzib, S. A.; Gong, Y.; Khan, Sophia; Medina, S-N. X.; Ortiz-León, Gisela N.; Reich, W.; Wyrowski, F.; Yang, A. Y.; Beuther, H.; Cotton, W. D.; Pandian, J. D.

doi:10.1051/0004-6361/202244115

Cited by 17 publications

(3 citation statements)

References 79 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The (l, v) distribution of H II regions and 6.7 GHz CH 3 OH masers, estimated to be at their far kinematic distances in Anderson et al (2014) and Nguyen et al (2022), reasonably well follow the Sagittarius and Perseus arms, at least down to Galactic longitudes of about 25°.…”

Section: Spiral Arm Assignmentsmentioning

confidence: 54%

On the Structure of the Sagittarius Spiral Arm in the Inner Milky Way

Bian,

Wu,

et al. 2024

Self Cite

View full text Add to dashboard Cite

We report measurements of trigonometric parallax and proper motion for two 6.7 GHz methanol and two 22 GHz water masers located in the far portion of the Sagittarius spiral arm as part of the BeSSeL Survey. Distances for these sources are estimated from parallax measurements combined with three-dimensional kinematic distances. The distances of G033.64−00.22, G035.57−00.03, G041.15−00.20, and G043.89−00.78 are 9.9 ± 0.5, 10.2 ± 0.6, 7.6 ± 0.5, and 7.5 ± 0.3 kpc, respectively. Based on these measurements, we suggest that the Sagittarius arm segment beyond about 8 kpc from the Sun in the first Galactic quadrant should be adjusted radially outward relative to previous models. This supports the suggestion of Xu et al. that the Sagittarius and Perseus spiral arms might merge in the first quadrant before spiraling inward to the far end of the Galactic bar.

show abstract

Section: Spiral Arm Assignmentsmentioning

confidence: 54%

On the Structure of the Sagittarius Spiral Arm in the Inner Milky Way

Bian,

Wu,

et al. 2024

Self Cite

View full text Add to dashboard Cite

show abstract

“…This makes the low-frequency radio window the most suitable to observe and study SNRs. The THOR and the GLOSTAR surveys have also been used to study the warm-ionized medium (Shanahan et al 2019), cloud formation processes (Wang et al 2020b), stellar feedback (Rugel et al 2019), OH and methanol masers (Beuther et al 2019;Ortiz-León et al 2021;Nguyen et al 2022), and the Galactic center star-formation rate (Nguyen et al 2021), to name a few. However, these centimetre wavelength surveys of the Milky Way lack an equivalent survey below 1 GHz (at wavelengths longer than 30 cm) that is sensitive to large-scale emission at arcsecond-level resolution covering the first quadrant of the Galactic plane.…”

Section: Introductionmentioning

confidence: 99%

Metrewave Galactic Plane with the uGMRT (MeGaPluG) Survey: Lessons from the pilot study

Dokara,

Roy,

Menten

et al. 2023

A&A

Self Cite

View full text Add to dashboard Cite

Context. The advent of wide-band receiver systems on interferometer arrays has enabled the undertaking of high-sensitivity and highresolution radio continuum surveys of the Galactic plane in a reasonable amount of telescope time. Yet, to date, there have been only a few such studies of the first quadrant of the Milky Way carried out at frequencies below 1 GHz. The Giant Metrewave Radio Telescope (GMRT) has recently upgraded its receivers with wide-band capabilities (now called the uGMRT), offering a prime opportunity to conduct high resolution surveys, while also demonstrating sensitivity to the extended structures. Aims. We wish to assess the feasibility of conducting a large-scale snapshot survey, the Metrewave Galactic Plane with the uGMRT Survey (MeGaPluG), to simultaneously map extended sources and compact objects at an angular resolution lower than 10″ and a point source sensitivity of 0.15 mJy beam−1. Methods. We performed an unbiased survey of a small portion of the Galactic plane, covering the W43/W44 regions (l = 29° – 35° and |b| < 1°) in two frequency bands: 300–500 MHz and 550–750 MHz. The 200 MHz wide-band receivers on the uGMRT were employed to observe the target field in several pointings, spending nearly 14 min on each pointing in two separate scans. We developed an automated pipeline for the calibration and a semi-automated self-calibration procedure was used to image each pointing using multi-scale CLEAN and outlier fields. Results. We produced continuum mosaics of the surveyed region at a final common resolution of 25″ in the two bands that have central frequencies of 400 MHz and 650 MHz, with a point source sensitivity better than 5 mJy beam−1. A spectral index map was also obtained, which is helpful to distinguish between thermal and nonthermal emission. By cross-matching with other surveys, we validated the positions and flux densities obtained from our data. We plan to cover a larger footprint of the Galactic plane in the near future based on the lessons drawn from this study.

show abstract

“…The image resulting from the combination of the VLA Darray and Effelsberg data of the pilot region is shown in Fig.5. The setup includes spectral windows covering the 6.7 GHz methanol maser transition(Ortiz-León et al 2021;Nguyen et al 2022), formaldehyde and radio recombination lines. Analysis of these data is still in the early stages but results are already starting to emerge (e.g.,Medina et al 2019;Nguyen et al 2021;Dokara et al 2021;Dzib et al 2023) that demonstrate the impact this survey will have in the future.…”

mentioning

confidence: 99%

Evolutionary Trends in Star Formation

Urquhart

2022

Proc. IAU

Self Cite

View full text Add to dashboard Cite

Over the past 20 years, the Galactic plane has been surveyed at high resolution at wavelengths from 1 micron through to 20 cm. The combination of these surveys has produced large samples of deeply embedded young stars located across the Galactic disc. These continuum surveys are complemented by spectral line surveys of thermal, radio recombination, and molecular maser (OH, H2O, CH3OH) lines. The identified sources cover the whole range of evolutionary stages in the star formation process, allowing the physical properties of these stages to be measured. This information has been used to calculate the star formation efficiency and star formation rate of the Milky Way and to evaluate the impact of environment and location within the disc. This review provides an overview of some of the most significant studies in recent years and discusses how the evolutionary sequence has been used to investigate the correlation of other star formation tracers and maser associations.

show abstract

A global view on star formation: The GLOSTAR Galactic plane survey

Cited by 17 publications

References 79 publications

On the Structure of the Sagittarius Spiral Arm in the Inner Milky Way

On the Structure of the Sagittarius Spiral Arm in the Inner Milky Way

Metrewave Galactic Plane with the uGMRT (MeGaPluG) Survey: Lessons from the pilot study

Evolutionary Trends in Star Formation

Contact Info

Product

Resources

About