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Journal articles on the topic 'HII regions;supernova remnants;radio lines'

Author: Grafiati

Published: 4 June 2021

Last updated: 20 February 2023

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1

Argo, M. K., A. Pedlar, T. W. B. Muxlow, and R. J. Beswick. "OH main line masers in the M 82 starburst." Proceedings of the International Astronomical Union 3, S242 (2007): 427–31. http://dx.doi.org/10.1017/s1743921307013543.

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AbstractA study of the distribution of OH gas in the central region of the nearby active starburst galaxy M82 has confirmed two previously known bright masers and revealed several new main line masers. Three of these are seen only at 1665 MHz, one is detected only at 1667 MHz, while the rest are detected in both lines. Observations covering both the 1665 and 1667 MHz lines, conducted with both the Very Large Array (VLA) and the Multi-Element Radio Linked Interferometer Network (MERLIN), have been used to accurately measure the positions and velocities of these features. This has allowed a comp

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Supan, L., G. Castelletti, W. M. Peters, and N. E. Kassim. "G51.04+0.07 and its environment: Identification of a new Galactic supernova remnant at low radio frequencies." Astronomy & Astrophysics 616 (August 2018): A98. http://dx.doi.org/10.1051/0004-6361/201832995.

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We have identified a new supernova remnant (SNR), G51.04+0.07, using observations at 74 MHz from the Very Large Array Low-Frequency Sky Survey Redux (VLSSr). Earlier, higher frequency radio continuum, recombination line, and infrared data had correctly inferred the presence of nonthermal radio emission within a larger, complex environment including ionised nebulae and active star formation. However, our observations have allowed us to redefine at least one SNR as a relatively small source (7.′5 × 3′in size) located at the southern periphery of the originally defined SNR candidate G51.21+0.11.

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3

Chu, You-Hua, and Robert C. Kennicutt. "Supernova Remnants in Giant HII Regions." International Astronomical Union Colloquium 101 (1988): 201–4. http://dx.doi.org/10.1017/s0252921100102374.

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Giant HII regions contain large numbers of massive stars, and hence are expected to contain large numbers of SNRs. Until recently, however, only a few SNRs have been identified in extragalactic giant HII regions. Moreover, most of these SNRs are located at the outskirts of HII regions, instead of the core where most of the stars are located. The low detection rate and the outlying locations of the SNRs may be due to: 1) observational difficulties - the background HII regions are much more luminous than the SNRs in both optical line emission and radio continuum; 2) intrinsic invisibility of SNR

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4

Filipović, M. D., L. Staveley-Smith, W. Reid, and P. A. Jones. "Supernova Remnants in the Magellanic Clouds." Symposium - International Astronomical Union 218 (2004): 87–88. http://dx.doi.org/10.1017/s0074180900180672.

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A study of the nature and the spatial distribution of over 250 discrete radio sources (HII regions and SNRs) in the Magellanic Clouds (MCs) is underway. A multi-frequency comparison of these sources involves the latest radio, IR, optical and X-ray surveys with angular resolution of <1′. Special emphasis is given to the MC SNRs. Their morphology, birth rate and overall properties are investigated and compared with Galactic SNRs and SNRs from other nearby galaxies. Also, we are investigating the radio source distribution throughout both MCs.

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5

Filipovic, M. D., P. A. Jones, and G. L. Vhite. "The relation between radio flux density and ionizing ultra-violet flux for HII regions and supernova remnants in the Large Magellanic cloud." Serbian Astronomical Journal, no. 166 (2003): 31–37. http://dx.doi.org/10.2298/saj0366031f.

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We present a comparison between the Parkes radio surveys (Filipovic et al 1995) and Vacuum Ultra-Violet (VUV) surveys (Smith et al. 1987) of the Large Magellanic Clouds (LMC). We have found 72 sources in common in the LMC which are known HII regions (52) and supernova remnants (SNRs) (19). Some of these radio sources are associated with two or more UV stellar associations. A comparison of the radio flux densities and ionizing UV flux for HII regions shows a very good correlation, as expected from theory. Many of the Magellanic Clouds (MCs) SNRs are embedded in HII regions, so there is also a r

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6

Odenwald, Sten F. "VLA Observations of Far-IR Sources Toward the Galactic Center." Symposium - International Astronomical Union 136 (1989): 205–11. http://dx.doi.org/10.1017/s0074180900186553.

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Preliminary results are presented from a 4.8-GHz VLA study of 5 far-IR sources within 1° of the Galactic center. Sgr-D and FIR-27 appear to be nearly featureless radio sources similar to young blister type HII regions, and FIR-21 has a filamentary structure similar to bright rimmed HII regions or Crab-like supernova remnants. Also presented are additional observations of Sgr-C.

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Filipović, Miroslav D., Paul A. Jones, Graeme L. White та Raymond F. Haynes. "Comparison of Discrete Sources in Radio and Hα Surveys of the Magellanic Clouds and the Potential for the New Hα Survey". Publications of the Astronomical Society of Australia 15, № 1 (1998): 128–31. http://dx.doi.org/10.1071/as98128.

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AbstractWe present a comparison between the latest Parkes radio surveys (Filipović et al. 1995, 1996, 1997) and Hα surveys of the Magellanic Clouds (Kennicutt & Hodge 1986). We have found 180 discrete sources in common for the Large Magellanic Cloud (LMC) and 40 in the field of the Small Magellanic Cloud (SMC). Most of these sources (95%) are HII regions and supernova remnants (SNRs). A comparison of the radio and Hα flux densities shows a very good correlation and we note that many of the Magellanic Clouds SNRs are embedded in HII regions.

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Turtle, A. J. "Supernova Remnants in the Magellanic Clouds Observed at the Molonglo Observatory." Symposium - International Astronomical Union 125 (1987): 130. http://dx.doi.org/10.1017/s0074180900160656.

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Radio surveys of the Magellanic Clouds at 843 MHz have been made with the Molonglo Observatory Synthesis Telescope. An initial catalogue (Mills et al. 1984) presented details of 38 supernova remnants detected by a combination of X-ray, optical and radio observations. The subsequent completion of the radio survey has revealed at least a further 17 remnants, mainly of large diameter and undetected by the Einstein X-ray Observatory. Though a few remnants have their radio emission concentrated towards their centre there is no evidence in the Magellanic Clouds for a Crab-like plerion (without an as

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9

Duncan, A. R., та R. F. Haynes. "Bright Prospects: Comparing the Hα Survey with Large-scale Radio Continuum Emission". Publications of the Astronomical Society of Australia 15, № 1 (1998): 50–55. http://dx.doi.org/10.1071/as98050.

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AbstractProspects for comparisons between the AAO/UKST Hα survey and large-scale radio continuum emission are considered, with particular reference to the recently completed Parkes 2·4 GHz survey of the southern Galactic Plane. Both these surveys have a high sensitivity to thermal emission, and comparisons between the Parkes work and previous Hα surveys show many objects in common. Possibilities for new detections include: a number of new supernova remnants; the faint extensions and envelopes surrounding ‘classical’ HII complexes, and other faint regions of thermal emission; several active HII

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10

Pedlar, Alan, Tom Muxlow, and Jon Riley. "Radio Observations of Supernova Remnants in the M82 Starburst." International Astronomical Union Colloquium 192 (2005): 219–25. http://dx.doi.org/10.1017/s0252921100009222.

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SummaryWe report on recent MERLIN, VLA and VLBI observations of the compact radio sources in the nearby starburst M82, with angular resolutions ranging from arcseconds to milliarcseconds. The spectral properties of the compact sources have been investigated by 15 GHz VLA-Pie Town observations which show that 16 of the less luminous compact sources are, in fact, HII regions. However the steep non-thermal spectrum, parsec size and small variability of the remaining sources is consistent with their being supernova remnants. Several show clear shell structures at MERLIN resolution (~50 mas) and 5

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11

HAN, J. L., W. REICH, X. H. SUN та ін. "THE SINO-GERMAN λ6 CM POLARIZATION SURVEY OF THE GALACTIC PLANE: A SUMMARY". International Journal of Modern Physics: Conference Series 23 (січень 2013): 82–91. http://dx.doi.org/10.1142/s2010194513011100.

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We have finished the λ6 cm polarization survey of the Galactic plane using the Urumqi 25 m radio telescope. It covers 10° ≤ l ≤ 230° in Galactic longitude and |b| ≤ 5° in Galactic latitude. The new polarization maps not only reveal new properties of the diffuse magnetized interstellar medium, but also are very useful for studying individual objects such as HII regions, which may act as Faraday screens with strong regular magnetic fields inside, and supernova remnants for their polarization properties and spectra. The high sensitivity of the survey enables us to discover two new SNRs G178.2–4.2

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12

Aksaker, Nazim, Sinan K. Yerli, Ümit Kızıloğlu, and Betül Atalay. "Emission Lines of Northern Planetary Nebulae." Proceedings of the International Astronomical Union 12, S323 (2016): 333–34. http://dx.doi.org/10.1017/s1743921317001909.

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AbstractIn this work, we present results of long slit spectrophotometric emission line flux observations of selected planetary nebulae (PNe). We have measured absolute fluxes and equivalent widths (EW) of all observable emission lines. In addition to these observations, electron temperatures (Te), densities (Ne), and chemical abundances were also calculated. The main purpose of this work is to fill the gaps in emission line flux standards for the northern hemisphere. It is expected that the measured fluxes would be used as standard data set for further photometric and spectrometric measurement

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13

Montmerle, Thierry. "Massive Stars and Giant HII Regions: The High-Energy Picture." Symposium - International Astronomical Union 143 (1991): 397–408. http://dx.doi.org/10.1017/s0074180900045502.

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Giant HII regions contain highly energetic objects: luminous, massive stars (including Wolf-Rayet stars) generating powerful winds, as well as, often, supernova remnants. These objects interact with the surrounding gas by creating shock waves. Part of the energy input is radiated away in the form of X-rays; also, protons and electrons may be accelerated in situ and generate γ-rays by collisions with the ionized gas. In addition, the stars themselves (including the accompanying low-mass PMS stars) are sources of X-rays, and W-R stars may emit continuum y-rays and are associated with nuclear γ-r

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14

Green, A. J. "The MOST Galactic Plane Survey." Publications of the Astronomical Society of Australia 14, no. 1 (1997): 73–76. http://dx.doi.org/10.1071/as97073.

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AbstractThe Molonglo Observatory Synthesis Telescope (MOST) has been upgraded to increase the diameter of the field of view from 70′ to 2·7°. A survey of the Galactic Plane is proposed to completely cover the region 240° ≤ l ≤ 365°, ∣ b ∣ ≤ 10° with a (1σ) sensitivity of 1–2 mJy. The results will provide a major resource for the investigation of supernova remnants, HII regions and transient radio sources. They will also be correlated with the galaxy search from the HI multibeam survey to be conducted at the Parkes telescope.

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15

Reich, W. "Radio Studies of Cosmic Rays in the Galaxy." Symposium - International Astronomical Union 144 (1991): 187–96. http://dx.doi.org/10.1017/s0074180900089063.

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Changes of the cosmic ray electron spectrum throughout the Galaxy have been found, based on the comparison of large-scale radio continuum surveys. These observations are not compatible with the assumption of a static Galactic halo, but indicate the existence of a Galactic wind. Galactic plane surveys reveal sources of cosmic ray electrons in the Galactic disk. Recent studies of the population of radio sources show no evidence for a large number of compact Galactic non-thermal sources. Most of the extended sources are probably HII-regions. Relatively few new supernova remnants (SNRs) with low s

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16

Wielebinski, R. "Radio Continuum Surveys Of The Sky." Symposium - International Astronomical Union 133 (1988): 323–29. http://dx.doi.org/10.1017/s0074180900139774.

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Radio continuum surveys give us the fundamental information about the distribution of the radio intensity across the sky. The radio waves originate in three fundamental emitting processes and are measured superposed in the antenna beam. At the lowest radio frequencies (below 10 GHz) the nonthermal emission process (synchrotron radiation) predominates. This radio emission comes from supernova remnants, from the “galactic background” (relativistic electrons diffusing in galactic magnetic fields), but also from extragalactic objects (galaxies, quasars, radio galaxies, etc.). In the frequency rang

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17

Vukotic, B., I. Bojicic, T. G. Pannuti, and Dejan Urosevic. "A search for candidate radio supernova remnants in the nearby irregular starburst galaxies NGC 4214 and NGC 4395." Serbian Astronomical Journal, no. 170 (2005): 101–10. http://dx.doi.org/10.2298/saj0570101v.

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We present the results of a search for new candidate radio su?pernova remnants (SNRs) in the nearby starburst irregular galaxies NGC 4214 and NGC 4395 using archived radio observations made with the Very Large Array (VLA) at the wavelengths of 3.5 cm, 6 cm and 20 cm for NGC 4214 and 6 cm and 20 cm for NGC 4395. These observations were analyzed as part of our ongoing search for candidate radio SNRs in nearby galaxies: the goal of this search is to prepare a large sample of candidate radio SNRs for the purpose of a robust statistical study of the properties of these sources. Based on our analysi

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18

Rosado, Margarita, Etienne le Coarer та Yvon Georgelin. "Results of the Hα Survey of the Small Magellanic Cloud". International Astronomical Union Colloquium 149 (1995): 150–54. http://dx.doi.org/10.1017/s0252921100022843.

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AbstractWe present the results of a kinematic survey of the Small Magellanic Cloud, performed with a scanning FP interferometer mainly at Hα. These data allow us to study the overall dynamics of the ionized hydrogen of this galaxy as well as the kinematics of classes of objects. In this presentation we exemplify how the availability of data in several wavelengths can be very useful in establishing the nature of large nebular complexes of the Small Magellanic Cloud. Our kinematic study allows us to discriminate faint shocked nebulae (such as supernova remnants) inside bright HII regions. This i

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19

Rosado, M., A. Bullejos, M. Valdez, et al. "Kinematics of the Ionized Gas in the Irregular Galaxies IC 10 and NGC 4449." Symposium - International Astronomical Union 190 (1999): 168–70. http://dx.doi.org/10.1017/s0074180900117796.

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We have searched for supernova remnants (SNRs) in the irregular galaxies IC 10 and NGC 4449 by means of Fabry-Perot interferometry in Hα and [SII] lines, complemented by radio continuum observations. We find several new SNR candidates in each galaxy in addition to the known ones. Although these galaxies have several common properties, the distributions of SNRs in each galaxy is different. This shows that the star formation mechanisms in these galaxies act in different ways, in favor of the formation of a large nebular HII complex in IC 10, similar to 30 Dor in the Large Magellanic Cloud. We ar

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20

Sofue, Yoshiaki. "Dark Supernova Remnants Revealed by CO-Line Bubbles in the W43 Molecular Complex along the 4-kpc Galactic Arm." Galaxies 9, no. 1 (2021): 13. http://dx.doi.org/10.3390/galaxies9010013.

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Fine structure of the density distribution in giant molecular clouds (GMCs) around W43 (G31+00+90 km s−1at ∼5.5 kpc) was analyzed using the FUGIN* CO-line survey at high-angular (20”∼0.5 pc) and velocity (1.3 km s−1) resolutions (*Four-receiver-system Unbiased Galactic Imaging survey with the Nobeyama 45-m telescope). The GMCs show highly turbulent structures, and the eddies are found to exhibit spherical bubble morphology appearing in narrow ranges of velocity channels. The bubbles are dark in radio continuum emission, unlike usual supernova remnants (SNR) or HII regions, and in infrared dust

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21

Sidorchuk, M. A., N. M. Vasilenko, O. M. Ulyanov, et al. "50 YEARS OF RESEARCH IN CONTINUUM AT THE UTR-2 RADIO TELESCOPE." Radio physics and radio astronomy 26, no. 4 (2021): 287–313. http://dx.doi.org/10.15407/rpra26.04.287.

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Purpose: The results of research in continuum decameter-wave radio emission of the Galaxy background, ionized hydrogen regions, supernova remnants, extragalactic discrete sources, extended galaxies, galactic clusters, extragalactic background are given. The aim of this work is reviewing the results achieved for over 50-years of the UTR-2 radiotelescope research of our Galaxy and its population, as well as extragalactic radio sources in the continuum radio emission spectrum at extremely low frequencies for the ground based observations. Design/methodology/approach: The review, analysis, collect

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22

Greenhouse, Matthew A., Uri Feldman, Howard A. Smith, Marcel Klapisch, Anand K. Bhatia, and Avi Bar-Shalom. "Infrared Coronal Emission Lines and the Possibility of their Laser Emission in Seyfert Nuclei." Symposium - International Astronomical Union 159 (1994): 447. http://dx.doi.org/10.1017/s0074180900176284.

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Infrared coronal emission lines are providing a new window for observation and analysis of highly ionized gas in Galactic and extragalactic sources such as Seyfert nuclei and classical novae shells. These lines are expected to be primary coolants in colliding galaxies, galaxy cluster cooling flows, cometary-compact HII regions, and supernova remnants. In this poster, we summarize results discussed in detail by Greenhouse et al. 1993, ApJS, 88, 23. We discuss approximately 74 infrared (1 < λ μm < 280) transitions within the ground configurations 2s22pk and 3s23pk (k = 1 to 5) or the first

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23

Lonsdale, Colin J., Katherine R. de Kleer, Philip J. Diamond, Hannah Thrall, Carol J. Lonsdale, and Harding E. Smith. "OH emission and absorption associated with supernovae in Arp 220." Proceedings of the International Astronomical Union 3, S242 (2007): 432–36. http://dx.doi.org/10.1017/s1743921307013555.

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AbstractWe present parsec-resolution spectral-line VLBI data for two epochs separated by 15 months as a precise new probe of the innermost regions of the nearby Ultraluminous Infrared Galaxy (ULIRG) Arp 220. This galaxy hosts a powerful starburst, with an associated supernova (SN) rate of order 4/yr. An extensive population of compact continuum sources interpreted as radio supernovae (RSNe) and young supernova remnants (SNR) has been imaged. We show here that many of the supernova-related radio continuum point sources exhibit clear evidence of OH absorption or maser emission in the intervening

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24

Hopp, Ulrich, H. U. Zimmermann, Manfred Stickel, and Christian Henkel. "A Supernova Remnant in the Dwarf HO IX." Symposium - International Astronomical Union 171 (1996): 392. http://dx.doi.org/10.1017/s0074180900233111.

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The dwarf irregular galaxy Ho IX (DDO 66) is a satellite of the giant spiral M81. Triggered by an interaction with M81 (Hopp & Schulte-Ladbeck, 1987 AA 187, 5), Ho IX may have recently undergone a burst of star formation. On very deep Calar Alto 3.5m telescope R images, we detected a ring-like nebula in the northeastern part of Ho IX, which is situated near to the giant CO molecular cloud recently discussed by Henkel et al. (1993 AA 273, L15). The structure of the nebula resembles supernova remnants like CTB 80. No HI-features can be detected at its location, especially no hole. It shows a

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25

Moorwood, A. F. M., and E. Oliva. "Infrared [FeII] and H2 Line Emission in Active Galactic Nuclei." Symposium - International Astronomical Union 134 (1989): 365–71. http://dx.doi.org/10.1017/s007418090014135x.

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Infrared spectra around [FeII](1.644μm), H2 (v = 1-0 S(1) at 2.121μm) and Brγ (H 7-4 at 2.167μm) have been obtained of 35 emission line nuclei whose optical spectra range from pure HII regionlike to Seyfert 1. All three emission lines have been detected in a large fraction of those nuclei exhibiting starburst activity but not in “pure” Seyferts. The highest detection frequency, however, was found for composite nuclei showing evidence for both starburst and Seyfert activity. Several arguments suggest that both the [FeII] and H2 are shock excited and could be largely attributed to supernova remn

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26

Corbelli, Edvige, Jonathan Braine, and Fatemeh S. Tabatabaei. "Radio emission during the formation of stellar clusters in M 33." Astronomy & Astrophysics 639 (July 2020): A27. http://dx.doi.org/10.1051/0004-6361/202037555.

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Aims. We investigate thermal and nonthermal radio emission associated with the early formation and evolution phases of young stellar clusters (YSCs) selected by their mid-infrared (MIR) emission at 24 μm in M 33. We consider regions in their early formation period, which are compact and totally embedded in the molecular cloud, and in the more evolved and exposed phase. Methods. Thanks to recent radio continuum surveys between 1.4 and 6.3 GHz we are able to find radio source counterparts to more than 300 star forming regions of M 33. We identify the thermal free–free component for YSCs and thei

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27

Hamza, Hasanein A., Ameerah Ab Al Sadooni, and Jacco Th van Loon. "Feedback from Ionized Outflows Traced Across the Nearly Edge-on Disk of the Nearby Seyfert 2 Galaxy NGC 4945*." NeuroQuantology 18, no. 12 (2020): 06–17. http://dx.doi.org/10.14704/nq.2020.18.12.nq20232.

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The aim of this work is to understand the impact of ionized outflows from H II regions in the nearby Seyfert 2 galaxy NGC4945. The study is based on long-slit optical spectra obtained at the Southern African large Telescope (SALT). The analysis focussed on recombination lines (Hα and Hβ) and forbidden lines ([N II]λλ6549,6583, [S II]λλ 6717,6731 and [O III] λλ4959,5007). The physical properties of 26 emission-line objects were determined from a diagnostic diagram. They are found to represent different physical environments normally encountered in supernova remnants, planetary nebulae (PNe) and

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28

Rennie, Thomas J., Stuart E. Harper, Clive Dickinson, et al. "COMAP Early Science. VI. A First Look at the COMAP Galactic Plane Survey." Astrophysical Journal 933, no. 2 (2022): 187. http://dx.doi.org/10.3847/1538-4357/ac63c8.

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Abstract We present early results from the CO Mapping Array Project (COMAP) Galactic Plane Survey conducted between 2019 June and 2021 April, spanning 20° < ℓ < 40° in Galactic longitude and ∣b∣ < 1.°5 in Galactic latitude with an angular resolution of 4.′5. We present initial results from the first part of the survey, including the diffuse emission and spectral energy distributions of H ii regions and supernova remnants (SNRs). Using low- and high-frequency surveys to constrain free–free and thermal dust emission contributions, we find evidence of excess flux density at 30 GHz in six

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