A Global View on Star Formation: The GLOSTAR Galactic Plane Survey. II. Supernova Remnants in the first quadrant of the Milky Way. (arXiv:2103.06267v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dokara_R/0/1/0/all/0/1">Rohit Dokara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brunthaler_A/0/1/0/all/0/1">A. Brunthaler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menten_K/0/1/0/all/0/1">K. M. Menten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dzib_S/0/1/0/all/0/1">S. A. Dzib</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reich_W/0/1/0/all/0/1">W. Reich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cotton_W/0/1/0/all/0/1">W. D. Cotton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_L/0/1/0/all/0/1">L. D. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_C/0/1/0/all/0/1">C. -H. R. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gong_Y/0/1/0/all/0/1">Y. Gong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Medina_S/0/1/0/all/0/1">S. -N. X. Medina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ortiz_Leon_G/0/1/0/all/0/1">G. N. Ortiz-León</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rugel_M/0/1/0/all/0/1">M. Rugel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Urquhart_J/0/1/0/all/0/1">J. S. Urquhart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wyrowski_F/0/1/0/all/0/1">F. Wyrowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_A/0/1/0/all/0/1">A. Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beuther_H/0/1/0/all/0/1">H. Beuther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Billington_S/0/1/0/all/0/1">S. J. Billington</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Csengeri_T/0/1/0/all/0/1">T. Csengeri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carrasco_Gonzalez_C/0/1/0/all/0/1">C. Carrasco-González</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roy_N/0/1/0/all/0/1">N. Roy</a>
Context. The properties of the population of the Galactic Supernova Remnants
(SNRs) are essential to our understanding of the dynamics of the Milky Way’s
interstellar medium (ISM). However, the completeness of the catalog of Galactic
SNRs is expected to be only ${sim}30%$, with on order 700 SNRs yet to be
detected. Deep interferometric radio continuum surveys of the Galactic plane
help in rectifying this apparent deficiency by identifying low surface
brightness SNRs and compact SNRs that have not been detected in previous
surveys. However, SNRs are routinely confused with H II regions, which can have
similar radio morphologies. Radio spectral index, polarization, and emission at
mid-infrared (MIR) wavelengths can help distinguish between SNRs and H II
regions.
Aims. We aim to identify SNR candidates using continuum emission from the
Karl G. Jansky Very Large Array Global view of the Star formation in the Milky
Way (GLOSTAR) survey.
Methods. GLOSTAR is a C-band (4–8 GHz) radio wavelength survey of the
Galactic plane covering $358<l<60, |b|<1$. The continuum images from this
survey that resulted from observations in the array’s most compact
configuration have an angular resolution of $18”$. We searched for SNRs in
these images to identify known SNRs, previously-identified SNR candidates and
new SNR candidates. We study these objects in MIR surveys and the GLOSTAR
polarization data to classify their emission as thermal or nonthermal.
Results. We identify 157 SNR candidates, out of which 80 are new.
Polarization measurements provide evidence of nonthermal emission from 9 of
these candidates. We find that two previously identified candidates are
filaments. We also detect emission from 91 out of 94 known SNRs in the survey
region. Four of these are reclassified as H II regions following detection in
MIR surveys.
(Abridged)
Context. The properties of the population of the Galactic Supernova Remnants
(SNRs) are essential to our understanding of the dynamics of the Milky Way’s
interstellar medium (ISM). However, the completeness of the catalog of Galactic
SNRs is expected to be only ${sim}30%$, with on order 700 SNRs yet to be
detected. Deep interferometric radio continuum surveys of the Galactic plane
help in rectifying this apparent deficiency by identifying low surface
brightness SNRs and compact SNRs that have not been detected in previous
surveys. However, SNRs are routinely confused with H II regions, which can have
similar radio morphologies. Radio spectral index, polarization, and emission at
mid-infrared (MIR) wavelengths can help distinguish between SNRs and H II
regions.
Aims. We aim to identify SNR candidates using continuum emission from the
Karl G. Jansky Very Large Array Global view of the Star formation in the Milky
Way (GLOSTAR) survey.
Methods. GLOSTAR is a C-band (4–8 GHz) radio wavelength survey of the
Galactic plane covering $358<l<60, |b|<1$. The continuum images from this
survey that resulted from observations in the array’s most compact
configuration have an angular resolution of $18”$. We searched for SNRs in
these images to identify known SNRs, previously-identified SNR candidates and
new SNR candidates. We study these objects in MIR surveys and the GLOSTAR
polarization data to classify their emission as thermal or nonthermal.
Results. We identify 157 SNR candidates, out of which 80 are new.
Polarization measurements provide evidence of nonthermal emission from 9 of
these candidates. We find that two previously identified candidates are
filaments. We also detect emission from 91 out of 94 known SNRs in the survey
region. Four of these are reclassified as H II regions following detection in
MIR surveys.
(Abridged)
http://arxiv.org/icons/sfx.gif
