C. Murugeshan, R. Džudžar, R. Bagge, T. O'Beirne, O. I. Wong, V. Kilborn, M. Cluver, K. Lutz, A. Elagali
Abstract We present a new high-resolution neutral atomic hydrogen (Hi) survey of ring galaxies using the Australia Telescope Compact Array (ATCA). We target a sample of 24 ring galaxies from the Buta (1995) Southern Ring Galaxy Survey Catalogue in order to study the origin of resonance-, collisional- and interaction-driven ring galaxies. In this work, we present an overview of the sample and study their global and resolved Hi properties. In addition, we also probe their star formation properties by measuring their star formation rates (SFR) and their resolved SFR surface density profiles. We find that a majority of the barred galaxies in our sample are Hi-deficient, alluding to the effects of the bar in driving their Hi deficiency. Furthermore, for the secularly evolving barred ring galaxies in our sample, we apply Lindblad’s resonance theory to predict the location of the resonance rings and find very good agreement between predictions and observations. We identify rings of Hi gas and/or star formation co-located at one or the other major resonances. Lastly, we measure the bar pattern speed ( $Omega_{textrm{bar}}$ ) for a sub-sample of our galaxies and find that the values range from 10–90 $textrm{km s}^{-1}$ kpc $^{-1}$ , in good agreement with previous studies.
{"title":"The Hi in Ring Galaxies Survey (Hi-RINGS)—Effects of the bar on the Hi gas in ring galaxies","authors":"C. Murugeshan, R. Džudžar, R. Bagge, T. O'Beirne, O. I. Wong, V. Kilborn, M. Cluver, K. Lutz, A. Elagali","doi":"10.1017/pasa.2023.19","DOIUrl":"https://doi.org/10.1017/pasa.2023.19","url":null,"abstract":"Abstract We present a new high-resolution neutral atomic hydrogen (Hi) survey of ring galaxies using the Australia Telescope Compact Array (ATCA). We target a sample of 24 ring galaxies from the Buta (1995) Southern Ring Galaxy Survey Catalogue in order to study the origin of resonance-, collisional- and interaction-driven ring galaxies. In this work, we present an overview of the sample and study their global and resolved Hi properties. In addition, we also probe their star formation properties by measuring their star formation rates (SFR) and their resolved SFR surface density profiles. We find that a majority of the barred galaxies in our sample are Hi-deficient, alluding to the effects of the bar in driving their Hi deficiency. Furthermore, for the secularly evolving barred ring galaxies in our sample, we apply Lindblad’s resonance theory to predict the location of the resonance rings and find very good agreement between predictions and observations. We identify rings of Hi gas and/or star formation co-located at one or the other major resonances. Lastly, we measure the bar pattern speed ( \u0000$Omega_{textrm{bar}}$\u0000 ) for a sub-sample of our galaxies and find that the values range from 10–90 \u0000$textrm{km s}^{-1}$\u0000 kpc \u0000$^{-1}$\u0000 , in good agreement with previous studies.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":"13 1","pages":""},"PeriodicalIF":6.3,"publicationDate":"2023-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"78387711","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Ashna Gulati, T. Murphy, D. Kaplan, R. Soria, J. Leung, Yuanming Wang, J. Pritchard, E. Lenc, S. Duchesne, A. O’Brien
Abstract We present a systematic search for radio counterparts of novae using the Australian Square Kilometer Array Pathfinder (ASKAP). Our search used the Rapid ASKAP Continuum Survey, which covered the entire sky south of declination $+41^{circ}$ ( $sim$ $34000$ square degrees) at a central frequency of 887.5 MHz, the Variables and Slow Transients Pilot Survey, which covered $sim$ $5000$ square degrees per epoch (887.5 MHz), and other ASKAP pilot surveys, which covered $sim$ 200–2000 square degrees with 2–12 h integration times. We crossmatched radio sources found in these surveys over a two–year period, from 2019 April to 2021 August, with 440 previously identified optical novae, and found radio counterparts for four novae: V5668 Sgr, V1369 Cen, YZ Ret, and RR Tel. Follow-up observations with the Australian Telescope Compact Array confirm the ejecta thinning across all observed bands with spectral analysis indicative of synchrotron emission in V1369 Cen and YZ Ret. Our light-curve fit with the Hubble Flow model yields a value of $1.65pm 0.17 times 10^{-4} rm :M_odot$ for the mass ejected in V1369 Cen. We also derive a peak surface brightness temperature of $250pm80$ K for YZ Ret. Using Hubble Flow model simulated radio lightcurves for novae, we demonstrate that with a 5 $sigma$ sensitivity limit of 1.5 mJy in 15-min survey observations, we can detect radio emission up to a distance of 4 kpc if ejecta mass is in the range $10^{-3}rm :M_odot$ , and upto 1 kpc if ejecta mass is in the range $10^{-5}$ – $10^{-3}rm :M_odot$ . Our study highlights ASKAP’s ability to contribute to future radio observations for novae within a distance of 1 kpc hosted on white dwarfs with masses $0.4$ – $1.25:rm M_odot$ , and within a distance of 4 kpc hosted on white dwarfs with masses $0.4$ – $1.0:rm M_odot$ .
{"title":"Classical novae in the ASKAP pilot surveys","authors":"Ashna Gulati, T. Murphy, D. Kaplan, R. Soria, J. Leung, Yuanming Wang, J. Pritchard, E. Lenc, S. Duchesne, A. O’Brien","doi":"10.1017/pasa.2023.21","DOIUrl":"https://doi.org/10.1017/pasa.2023.21","url":null,"abstract":"Abstract We present a systematic search for radio counterparts of novae using the Australian Square Kilometer Array Pathfinder (ASKAP). Our search used the Rapid ASKAP Continuum Survey, which covered the entire sky south of declination \u0000$+41^{circ}$\u0000 ( \u0000$sim$\u0000 \u0000$34000$\u0000 square degrees) at a central frequency of 887.5 MHz, the Variables and Slow Transients Pilot Survey, which covered \u0000$sim$\u0000 \u0000$5000$\u0000 square degrees per epoch (887.5 MHz), and other ASKAP pilot surveys, which covered \u0000$sim$\u0000 200–2000 square degrees with 2–12 h integration times. We crossmatched radio sources found in these surveys over a two–year period, from 2019 April to 2021 August, with 440 previously identified optical novae, and found radio counterparts for four novae: V5668 Sgr, V1369 Cen, YZ Ret, and RR Tel. Follow-up observations with the Australian Telescope Compact Array confirm the ejecta thinning across all observed bands with spectral analysis indicative of synchrotron emission in V1369 Cen and YZ Ret. Our light-curve fit with the Hubble Flow model yields a value of \u0000$1.65pm 0.17 times 10^{-4} rm :M_odot$\u0000 for the mass ejected in V1369 Cen. We also derive a peak surface brightness temperature of \u0000$250pm80$\u0000 K for YZ Ret. Using Hubble Flow model simulated radio lightcurves for novae, we demonstrate that with a 5 \u0000$sigma$\u0000 sensitivity limit of 1.5 mJy in 15-min survey observations, we can detect radio emission up to a distance of 4 kpc if ejecta mass is in the range \u0000$10^{-3}rm :M_odot$\u0000 , and upto 1 kpc if ejecta mass is in the range \u0000$10^{-5}$\u0000 – \u0000$10^{-3}rm :M_odot$\u0000 . Our study highlights ASKAP’s ability to contribute to future radio observations for novae within a distance of 1 kpc hosted on white dwarfs with masses \u0000$0.4$\u0000 – \u0000$1.25:rm M_odot$\u0000 , and within a distance of 4 kpc hosted on white dwarfs with masses \u0000$0.4$\u0000 – \u0000$1.0:rm M_odot$\u0000 .","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":"12 1","pages":""},"PeriodicalIF":6.3,"publicationDate":"2023-03-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"85237905","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
I. Morrison, B. Crosse, G. Sleap, R. Wayth, A. Williams, M. Johnston-Hollitt, J. Jones, S. Tingay, M. Walker, L. Williams
Abstract We describe the design, validation, and commissioning of a new correlator termed ‘MWAX’ for the Murchison Widefield Array (MWA) low-frequency radio telescope. MWAX replaces an earlier generation MWA correlator, extending correlation capabilities and providing greater flexibility, scalability, and maintainability. MWAX is designed to exploit current and future Phase II/III upgrades to MWA infrastructure, most notably the simultaneous correlation of all 256 of the MWA’s antenna tiles (and potentially more in future). MWAX is a fully software-programmable correlator based around an ethernet multicast architecture. At its core is a cluster of 24 high-performance GPU-enabled commercial-off-the-shelf compute servers that together process in real-time up to 24 coarse channels of 1.28 MHz bandwidth each. The system is highly flexible and scalable in terms of the number of antenna tiles and number of coarse channels to be correlated, and it offers a wide range of frequency/time resolution combinations to users. We conclude with a roadmap of future enhancements and extensions that we anticipate will be progressively rolled out over time.
{"title":"MWAX: A new correlator for the Murchison Widefield Array","authors":"I. Morrison, B. Crosse, G. Sleap, R. Wayth, A. Williams, M. Johnston-Hollitt, J. Jones, S. Tingay, M. Walker, L. Williams","doi":"10.1017/pasa.2023.15","DOIUrl":"https://doi.org/10.1017/pasa.2023.15","url":null,"abstract":"Abstract We describe the design, validation, and commissioning of a new correlator termed ‘MWAX’ for the Murchison Widefield Array (MWA) low-frequency radio telescope. MWAX replaces an earlier generation MWA correlator, extending correlation capabilities and providing greater flexibility, scalability, and maintainability. MWAX is designed to exploit current and future Phase II/III upgrades to MWA infrastructure, most notably the simultaneous correlation of all 256 of the MWA’s antenna tiles (and potentially more in future). MWAX is a fully software-programmable correlator based around an ethernet multicast architecture. At its core is a cluster of 24 high-performance GPU-enabled commercial-off-the-shelf compute servers that together process in real-time up to 24 coarse channels of 1.28 MHz bandwidth each. The system is highly flexible and scalable in terms of the number of antenna tiles and number of coarse channels to be correlated, and it offers a wide range of frequency/time resolution combinations to users. We conclude with a roadmap of future enhancements and extensions that we anticipate will be progressively rolled out over time.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":"23 1","pages":""},"PeriodicalIF":6.3,"publicationDate":"2023-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"87295041","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
A. Watts, L. Cortese, B. Catinella, T. Brown, C. Wilson, N. Zabel, I. Roberts, T. Davis, M. Thorp, A. Chung, A. Stevens, S. Ellison, K. Spekkens, L. Parker, Y. M. Bahé, V. Villanueva, M. Jimenez-Donaire, D. Bisaria, A. Boselli, A. Bolatto, Bumhyun Lee
Abstract The quenching of cluster satellite galaxies is inextricably linked to the suppression of their cold interstellar medium (ISM) by environmental mechanisms. While the removal of neutral atomic hydrogen (H i) at large radii is well studied, how the environment impacts the remaining gas in the centres of galaxies, which are dominated by molecular gas, is less clear. Using new observations from the Virgo Environment traced in CO survey (VERTICO) and archival H i data, we study the H i and molecular gas within the optical discs of Virgo cluster galaxies on 1.2-kpc scales with spatially resolved scaling relations between stellar ( $Sigma_{star}$ ), H i ( $Sigma_{text{H},{smalltext{I}}}$ ), and molecular gas ( $Sigma_{text{mol}}$ ) surface densities. Adopting H i deficiency as a measure of environmental impact, we find evidence that, in addition to removing the H i at large radii, the cluster processes also lower the average $Sigma_{text{H},{smalltext{I}}}$ of the remaining gas even in the central $1.2,$ kpc. The impact on molecular gas is comparatively weaker than on the H i, and we show that the lower $Sigma_{text{mol}}$ gas is removed first. In the most H i-deficient galaxies, however, we find evidence that environmental processes reduce the typical $Sigma_{text{mol}}$ of the remaining gas by nearly a factor of 3. We find no evidence for environment-driven elevation of $Sigma_{text{H},{smalltext{I}}}$ or $Sigma_{text{mol}}$ in H i-deficient galaxies. Using the ratio of $Sigma_{text{mol}}$ -to- $Sigma_{text{H},{smalltext{I}}}$ in individual regions, we show that changes in the ISM physical conditions, estimated using the total gas surface density and midplane hydrostatic pressure, cannot explain the observed reduction in molecular gas content. Instead, we suggest that direct stripping of the molecular gas is required to explain our results.
{"title":"VERTICO V: The environmentally driven evolution of the inner cold gas discs of Virgo cluster galaxies","authors":"A. Watts, L. Cortese, B. Catinella, T. Brown, C. Wilson, N. Zabel, I. Roberts, T. Davis, M. Thorp, A. Chung, A. Stevens, S. Ellison, K. Spekkens, L. Parker, Y. M. Bahé, V. Villanueva, M. Jimenez-Donaire, D. Bisaria, A. Boselli, A. Bolatto, Bumhyun Lee","doi":"10.1017/pasa.2023.14","DOIUrl":"https://doi.org/10.1017/pasa.2023.14","url":null,"abstract":"Abstract The quenching of cluster satellite galaxies is inextricably linked to the suppression of their cold interstellar medium (ISM) by environmental mechanisms. While the removal of neutral atomic hydrogen (H i) at large radii is well studied, how the environment impacts the remaining gas in the centres of galaxies, which are dominated by molecular gas, is less clear. Using new observations from the Virgo Environment traced in CO survey (VERTICO) and archival H i data, we study the H i and molecular gas within the optical discs of Virgo cluster galaxies on 1.2-kpc scales with spatially resolved scaling relations between stellar ( \u0000$Sigma_{star}$\u0000 ), H i ( \u0000$Sigma_{text{H},{smalltext{I}}}$\u0000 ), and molecular gas ( \u0000$Sigma_{text{mol}}$\u0000 ) surface densities. Adopting H i deficiency as a measure of environmental impact, we find evidence that, in addition to removing the H i at large radii, the cluster processes also lower the average \u0000$Sigma_{text{H},{smalltext{I}}}$\u0000 of the remaining gas even in the central \u0000$1.2,$\u0000 kpc. The impact on molecular gas is comparatively weaker than on the H i, and we show that the lower \u0000$Sigma_{text{mol}}$\u0000 gas is removed first. In the most H i-deficient galaxies, however, we find evidence that environmental processes reduce the typical \u0000$Sigma_{text{mol}}$\u0000 of the remaining gas by nearly a factor of 3. We find no evidence for environment-driven elevation of \u0000$Sigma_{text{H},{smalltext{I}}}$\u0000 or \u0000$Sigma_{text{mol}}$\u0000 in H i-deficient galaxies. Using the ratio of \u0000$Sigma_{text{mol}}$\u0000 -to- \u0000$Sigma_{text{H},{smalltext{I}}}$\u0000 in individual regions, we show that changes in the ISM physical conditions, estimated using the total gas surface density and midplane hydrostatic pressure, cannot explain the observed reduction in molecular gas content. Instead, we suggest that direct stripping of the molecular gas is required to explain our results.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":"24 10","pages":""},"PeriodicalIF":6.3,"publicationDate":"2023-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"72409697","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
A. C. R. Gomes, A. C. Souza, A. Jasper, B. R. Galvão
Abstract Phosphorus nitride (PN) is believed to be one of the major reservoirs of phosphorus in the interstellar medium (ISM). For this reason, understanding which reactions produce PN in space and predicting their rate coefficients is important for modelling the relative abundances of P-bearing species and clarifying the role of phosphorus in astrochemistry. In this work, we explore the potential energy surfaces of the $textrm{P}(^4textrm{S}) + textrm{NH}(^3Sigma^-)$ and $textrm{N}(^4textrm{S}) + textrm{PH}(^3Sigma^-)$ reactions and the formation of $textrm{H}(^2textrm{S}) + textrm{PN}(^1Sigma^+)$ through high accuracy ab initio calculations and the variable reaction coordinate transition state theory (VRC-TST). We found that both reactions proceed without an activation barrier and with similar rate coefficients that can be described by a modified Arrhenius equation ( $k(T)=alpha!left( T/300 right)^{beta} exp!{(!-!gamma/T)})$ with $alpha=0.93times 10^{-10}rm cm^3,s^{-1}$ , $beta=-0.18$ and $gamma=0.24, rm K$ for the $textrm{P} + textrm{NH} longrightarrow textrm{H} + textrm{PN}$ reaction and $alpha=0.88times 10^{-10}rm cm^3,s^{-1}$ , $beta=-0.18$ and $gamma=1.01, rm K$ for the $textrm{N} + textrm{PH} longrightarrow textrm{H} + textrm{PN}$ one. Both reactions are expected to be relevant for modelling PN abundances even in the cold environments of the ISM. Given the abundance of hydrogen in space, we have also predicted rate coefficients for the destruction of PN via H + PN collisions.
{"title":"The P(4S) + NH(3Σ–) and N(4S) + PH(3Σ–)reactions as sources of interstellar phosphorus nitride","authors":"A. C. R. Gomes, A. C. Souza, A. Jasper, B. R. Galvão","doi":"10.1017/pasa.2023.13","DOIUrl":"https://doi.org/10.1017/pasa.2023.13","url":null,"abstract":"Abstract Phosphorus nitride (PN) is believed to be one of the major reservoirs of phosphorus in the interstellar medium (ISM). For this reason, understanding which reactions produce PN in space and predicting their rate coefficients is important for modelling the relative abundances of P-bearing species and clarifying the role of phosphorus in astrochemistry. In this work, we explore the potential energy surfaces of the \u0000$textrm{P}(^4textrm{S}) + textrm{NH}(^3Sigma^-)$\u0000 and \u0000$textrm{N}(^4textrm{S}) + textrm{PH}(^3Sigma^-)$\u0000 reactions and the formation of \u0000$textrm{H}(^2textrm{S}) + textrm{PN}(^1Sigma^+)$\u0000 through high accuracy ab initio calculations and the variable reaction coordinate transition state theory (VRC-TST). We found that both reactions proceed without an activation barrier and with similar rate coefficients that can be described by a modified Arrhenius equation ( \u0000$k(T)=alpha!left( T/300 right)^{beta} exp!{(!-!gamma/T)})$\u0000 with \u0000$alpha=0.93times 10^{-10}rm cm^3,s^{-1}$\u0000 , \u0000$beta=-0.18$\u0000 and \u0000$gamma=0.24, rm K$\u0000 for the \u0000$textrm{P} + textrm{NH} longrightarrow textrm{H} + textrm{PN}$\u0000 reaction and \u0000$alpha=0.88times 10^{-10}rm cm^3,s^{-1}$\u0000 , \u0000$beta=-0.18$\u0000 and \u0000$gamma=1.01, rm K$\u0000 for the \u0000$textrm{N} + textrm{PH} longrightarrow textrm{H} + textrm{PN}$\u0000 one. Both reactions are expected to be relevant for modelling PN abundances even in the cold environments of the ISM. Given the abundance of hydrogen in space, we have also predicted rate coefficients for the destruction of PN via H + PN collisions.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":"20 1","pages":""},"PeriodicalIF":6.3,"publicationDate":"2023-03-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"77968301","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
J. A. Grundy, O. I. Wong, K. Lee-Waddell, N. Seymour, B. For, C. Murugeshan, B. Koribalski, J. Madrid, J. Rhee, T. Westmeier
Abstract We present the highest resolution and sensitivity $sim$ $1.4,$ GHz continuum observations of the Eridanus supergroup obtained as a part of the Widefield Australian Square Kilometer Array Pathfinder (ASKAP) L-band Legacy All-sky Blind surveY (WALLABY) pre-pilot observations using the ASKAP. We detect 9461 sources at 1.37 GHz down to a flux density limit of $sim$ $0.1$ mJy at $6.1''times 7.9''$ resolution with a median root mean square of 0.05 mJy beam $^{-1}$ . We find that the flux scale is accurate to within 5 % (compared to NVSS at 1.4 GHz). We then determine the global properties of eight Eridanus supergroup members, which are detected in both radio continuum and neutral hydrogen (HI) emission, and find that the radio-derived star formation rates (SFRs) agree well with previous literature. Using our global and resolved radio continuum properties of the nearby Eridanus galaxies, we measure and extend the infrared-radio correlation (IRRC) to lower stellar masses and inferred SFRs than before. We find the resolved IRRC to be useful for: (1) discriminating between active galactic nuclei and star-forming galaxies; (2) identifying background radio sources; and (3) tracing the effects of group environment pre-processing in NGC 1385. We find evidence for tidal interactions and ram-pressure stripping in the HI, resolved spectral index and IRRC morphologies of NGC 1385. There appears to be a spatial coincidence (in projection) of double-lobed radio jets with the central HI hole of NGC 1367. The destruction of polycyclic aromatic hydrocarbons by merger-induced shocks may be driving the observed WISE W3 deficit observed in NGC 1359. Our results suggest that resolved radio continuum and IRRC studies are excellent tracers of the physical processes that drive galaxy evolution and will be possible on larger sample of sources with upcoming ASKAP radio continuum surveys.
{"title":"WALLABY pre-pilot survey: Radio continuum properties of the Eridanus supergroup","authors":"J. A. Grundy, O. I. Wong, K. Lee-Waddell, N. Seymour, B. For, C. Murugeshan, B. Koribalski, J. Madrid, J. Rhee, T. Westmeier","doi":"10.1017/pasa.2023.11","DOIUrl":"https://doi.org/10.1017/pasa.2023.11","url":null,"abstract":"Abstract We present the highest resolution and sensitivity \u0000$sim$\u0000 \u0000$1.4,$\u0000 GHz continuum observations of the Eridanus supergroup obtained as a part of the Widefield Australian Square Kilometer Array Pathfinder (ASKAP) L-band Legacy All-sky Blind surveY (WALLABY) pre-pilot observations using the ASKAP. We detect 9461 sources at 1.37 GHz down to a flux density limit of \u0000$sim$\u0000 \u0000$0.1$\u0000 mJy at \u0000$6.1''times 7.9''$\u0000 resolution with a median root mean square of 0.05 mJy beam \u0000$^{-1}$\u0000 . We find that the flux scale is accurate to within 5 % (compared to NVSS at 1.4 GHz). We then determine the global properties of eight Eridanus supergroup members, which are detected in both radio continuum and neutral hydrogen (HI) emission, and find that the radio-derived star formation rates (SFRs) agree well with previous literature. Using our global and resolved radio continuum properties of the nearby Eridanus galaxies, we measure and extend the infrared-radio correlation (IRRC) to lower stellar masses and inferred SFRs than before. We find the resolved IRRC to be useful for: (1) discriminating between active galactic nuclei and star-forming galaxies; (2) identifying background radio sources; and (3) tracing the effects of group environment pre-processing in NGC 1385. We find evidence for tidal interactions and ram-pressure stripping in the HI, resolved spectral index and IRRC morphologies of NGC 1385. There appears to be a spatial coincidence (in projection) of double-lobed radio jets with the central HI hole of NGC 1367. The destruction of polycyclic aromatic hydrocarbons by merger-induced shocks may be driving the observed WISE W3 deficit observed in NGC 1359. Our results suggest that resolved radio continuum and IRRC studies are excellent tracers of the physical processes that drive galaxy evolution and will be possible on larger sample of sources with upcoming ASKAP radio continuum surveys.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":"32 1","pages":""},"PeriodicalIF":6.3,"publicationDate":"2023-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79006796","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
N. Bhat, N. A. Swainston, S. McSweeney, M. Xue, B. W. Meyers, S. Kudale, S. Dai, S. Tremblay, W. van Straten, R. Shannon, K. R. Smith, M. Sokolowski, S. Ord, G. Sleap, A. Williams, P. Hancock, R. Lange, J. Tocknell, M. Johnston-Hollitt, D. Kaplan, S. Tingay, M. Walker
Abstract We present an overview of the Southern-sky MWA Rapid Two-metre (SMART) pulsar survey that exploits the Murchison Widefield Array’s large field of view and voltage-capture system to survey the sky south of 30 $^{circ}$ in declination for pulsars and fast transients in the 140–170 MHz band. The survey is enabled by the advent of the Phase II MWA’s compact configuration, which offers an enormous efficiency in beam-forming and processing costs, thereby making an all-sky survey of this magnitude tractable with the MWA. Even with the long dwell times employed for the survey (4800 s), data collection can be completed in $<$ 100 h of telescope time, while still retaining the ability to reach a limiting sensitivity of $sim$ 2–3 mJy (at 150 MHz, near zenith), which is effectively 3–5 times deeper than the previous-generation low-frequency southern-sky pulsar survey, completed in the 1990s. Each observation is processed to generate $sim$ 5000–8000 tied-array beams that tessellate the full $sim 610, {textrm{deg}^{2}}$ field of view (at 155 MHz), which are then processed to search for pulsars. The voltage-capture recording of the survey also allows a multitude of post hoc processing options including the reprocessing of data for higher time resolution and even exploring image-based techniques for pulsar candidate identification. Due to the substantial computational cost in pulsar searches at low frequencies, the survey data processing is undertaken in multiple passes: in the first pass, a shallow survey is performed, where 10 min of each observation is processed, reaching about one-third of the full-search sensitivity. Here we present the system overview including details of ongoing processing and initial results. Further details including first pulsar discoveries and a census of low-frequency detections are presented in a companion paper. Future plans include deeper searches to reach the full sensitivity and acceleration searches to target binary and millisecond pulsars. Our simulation analysis forecasts $sim$ 300 new pulsars upon the completion of full processing. The SMART survey will also generate a complete digital record of the low-frequency sky, which will serve as a valuable reference for future pulsar searches planned with the low-frequency Square Kilometre Array.
{"title":"The Southern-sky MWA Rapid Two-metre (SMART) pulsar survey—I. Survey design and processing pipeline","authors":"N. Bhat, N. A. Swainston, S. McSweeney, M. Xue, B. W. Meyers, S. Kudale, S. Dai, S. Tremblay, W. van Straten, R. Shannon, K. R. Smith, M. Sokolowski, S. Ord, G. Sleap, A. Williams, P. Hancock, R. Lange, J. Tocknell, M. Johnston-Hollitt, D. Kaplan, S. Tingay, M. Walker","doi":"10.1017/pasa.2023.17","DOIUrl":"https://doi.org/10.1017/pasa.2023.17","url":null,"abstract":"Abstract We present an overview of the Southern-sky MWA Rapid Two-metre (SMART) pulsar survey that exploits the Murchison Widefield Array’s large field of view and voltage-capture system to survey the sky south of 30 \u0000$^{circ}$\u0000 in declination for pulsars and fast transients in the 140–170 MHz band. The survey is enabled by the advent of the Phase II MWA’s compact configuration, which offers an enormous efficiency in beam-forming and processing costs, thereby making an all-sky survey of this magnitude tractable with the MWA. Even with the long dwell times employed for the survey (4800 s), data collection can be completed in \u0000$<$\u0000 100 h of telescope time, while still retaining the ability to reach a limiting sensitivity of \u0000$sim$\u0000 2–3 mJy (at 150 MHz, near zenith), which is effectively 3–5 times deeper than the previous-generation low-frequency southern-sky pulsar survey, completed in the 1990s. Each observation is processed to generate \u0000$sim$\u0000 5000–8000 tied-array beams that tessellate the full \u0000$sim 610, {textrm{deg}^{2}}$\u0000 field of view (at 155 MHz), which are then processed to search for pulsars. The voltage-capture recording of the survey also allows a multitude of post hoc processing options including the reprocessing of data for higher time resolution and even exploring image-based techniques for pulsar candidate identification. Due to the substantial computational cost in pulsar searches at low frequencies, the survey data processing is undertaken in multiple passes: in the first pass, a shallow survey is performed, where 10 min of each observation is processed, reaching about one-third of the full-search sensitivity. Here we present the system overview including details of ongoing processing and initial results. Further details including first pulsar discoveries and a census of low-frequency detections are presented in a companion paper. Future plans include deeper searches to reach the full sensitivity and acceleration searches to target binary and millisecond pulsars. Our simulation analysis forecasts \u0000$sim$\u0000 300 new pulsars upon the completion of full processing. The SMART survey will also generate a complete digital record of the low-frequency sky, which will serve as a valuable reference for future pulsar searches planned with the low-frequency Square Kilometre Array.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":"12 1","pages":""},"PeriodicalIF":6.3,"publicationDate":"2023-02-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"87532571","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
N. Bhat, N. A. Swainston, S. McSweeney, M. Xue, B. W. Meyers, S. Kudale, S. Dai, S. Tremblay, W. van Straten, R. Shannon, K. R. Smith, M. Sokolowski, S. Ord, G. Sleap, A. Williams, P. Hancock, R. Lange, J. Tocknell, M. Johnston-Hollitt, D. Kaplan, S. Tingay, M. Walker
Abstract In Paper I, we presented an overview of the Southern-sky MWA Rapid Two-metre (SMART) survey, including the survey design and search pipeline. While the combination of MWA’s large field-of-view and the voltage capture system brings a survey speed of ${sim} 450, {textrm{deg}}^{2},textrm{h}^{-1}$ , the progression of the survey relies on the availability of compact configuration of the Phase II array. Over the past few years, by taking advantage of multiple windows of opportunity when the compact configuration was available, we have advanced the survey to 75% of the planned sky coverage. To date, about 10% of the data collected thus far have been processed for a first-pass search, where 10 min of observation is processed for dispersion measures out to 250 ${textrm{pc cm}}^{-3}$ , to realise a shallow survey that is largely sensitive to long-period pulsars. The ongoing analysis has led to two new pulsar discoveries, as well as an independent discovery and a rediscovery of a previously incorrectly characterised pulsar, all from ${sim} 3% $ of the data for which candidate scrutiny is completed. In this sequel to Paper I, we describe the strategies for further detailed follow-up including improved sky localisation and convergence to timing solution, and illustrate them using example pulsar discoveries. The processing has also led to re-detection of 120 pulsars in the SMART observing band, bringing the total number of pulsars detected to date with the MWA to 180, and these are used to assess the search sensitivity of current processing pipelines. The planned second-pass (deep survey) processing is expected to yield a three-fold increase in sensitivity for long-period pulsars, and a substantial improvement to millisecond pulsars by adopting optimal de-dispersion plans. The SMART survey will complement the highly successful Parkes High Time Resolution Universe survey at 1.2–1.5 GHz, and inform future large survey efforts such as those planned with the low-frequency Square Kilometre Array (SKA-Low).
{"title":"The Southern-sky MWA Rapid Two-metre (SMART) pulsar survey—II. Survey status, pulsar census, and first pulsar discoveries","authors":"N. Bhat, N. A. Swainston, S. McSweeney, M. Xue, B. W. Meyers, S. Kudale, S. Dai, S. Tremblay, W. van Straten, R. Shannon, K. R. Smith, M. Sokolowski, S. Ord, G. Sleap, A. Williams, P. Hancock, R. Lange, J. Tocknell, M. Johnston-Hollitt, D. Kaplan, S. Tingay, M. Walker","doi":"10.1017/pasa.2023.18","DOIUrl":"https://doi.org/10.1017/pasa.2023.18","url":null,"abstract":"Abstract In Paper I, we presented an overview of the Southern-sky MWA Rapid Two-metre (SMART) survey, including the survey design and search pipeline. While the combination of MWA’s large field-of-view and the voltage capture system brings a survey speed of \u0000${sim} 450, {textrm{deg}}^{2},textrm{h}^{-1}$\u0000 , the progression of the survey relies on the availability of compact configuration of the Phase II array. Over the past few years, by taking advantage of multiple windows of opportunity when the compact configuration was available, we have advanced the survey to 75% of the planned sky coverage. To date, about 10% of the data collected thus far have been processed for a first-pass search, where 10 min of observation is processed for dispersion measures out to 250 \u0000${textrm{pc cm}}^{-3}$\u0000 , to realise a shallow survey that is largely sensitive to long-period pulsars. The ongoing analysis has led to two new pulsar discoveries, as well as an independent discovery and a rediscovery of a previously incorrectly characterised pulsar, all from \u0000${sim} 3% $\u0000 of the data for which candidate scrutiny is completed. In this sequel to Paper I, we describe the strategies for further detailed follow-up including improved sky localisation and convergence to timing solution, and illustrate them using example pulsar discoveries. The processing has also led to re-detection of 120 pulsars in the SMART observing band, bringing the total number of pulsars detected to date with the MWA to 180, and these are used to assess the search sensitivity of current processing pipelines. The planned second-pass (deep survey) processing is expected to yield a three-fold increase in sensitivity for long-period pulsars, and a substantial improvement to millisecond pulsars by adopting optimal de-dispersion plans. The SMART survey will complement the highly successful Parkes High Time Resolution Universe survey at 1.2–1.5 GHz, and inform future large survey efforts such as those planned with the low-frequency Square Kilometre Array (SKA-Low).","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":"146 1","pages":""},"PeriodicalIF":6.3,"publicationDate":"2023-02-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"88637548","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Anita Petzler, J. Dawson, Hiep Nguyen, C. Heiles, M. Wardle, M.-Y. Lee, C. Murray, K. Thompson, S. Stanimirović
Abstract We present observations of the four $^2 Pi _{3/2},J=3/2$ ground-rotational state transitions of the hydroxyl molecule (OH) along 107 lines of sight both in and out of the Galactic plane: 92 sets of observations from the Arecibo telescope and 15 sets of observations from the Australia Telescope Compact Array (ATCA). Our Arecibo observations included off-source pointings, allowing us to measure excitation temperature ( $T_{rm ex}$ ) and optical depth, while our ATCA observations give optical depth only. We perform Gaussian decomposition using the Automated Molecular Excitation Bayesian line-fitting Algorithm ‘Amoeba’ (Petzler, Dawson, & Wardle 2021, ApJ, 923, 261) fitting all four transitions simultaneously with shared centroid velocity and width. We identify 109 features across 38 sightlines (including 58 detections along 27 sightlines with excitation temperature measurements). While the main lines at 1665 and 1667 MHz tend to have similar excitation temperatures (median $|Delta T_{rm ex}({rm main})|=0.6,$ K, 84% show $|Delta T_{rm ex}({rm main})|<2,$ K), large differences in the 1612 and 1720 MHz satellite line excitation temperatures show that the gas is generally not in LTE. For a selection of sightlines, we compare our OH features to associated (on-sky and in velocity) Hi cold gas components (CNM) identified by Nguyen et al. (2019, ApJ, 880, 141) and find no strong correlations. We speculate that this may indicate an effective decoupling of the molecular gas from the CNM once it accumulates.
摘要:我们在银河面内外的107条视线上对羟基分子(OH)的4次$^2 Pi _{3/2},J=3/2$地旋态跃迁进行了观测，其中92组观测来自阿雷西博望远镜，15组观测来自澳大利亚望远镜紧凑阵列(ATCA)。我们的阿雷西博观测包括非源点，允许我们测量激发温度($T_{rm ex}$)和光学深度，而我们的ATCA观测只给出光学深度。我们使用自动分子激发贝叶斯线拟合算法“Amoeba”(Petzler, Dawson， ＆ Wardle 2021, ApJ, 923, 261)进行高斯分解，同时拟合所有四个过渡，共享质心速度和宽度。我们确定了38条视线中的109个特征(包括沿27条视线的58个探测，并测量了激发温度)。而1665和1667 MHz的主线往往具有相似的激发温度(中位数$|Delta T_{rm ex}({rm main})|=0.6,$ K, 84)% show $|Delta T_{rm ex}({rm main})|<2,$ K), large differences in the 1612 and 1720 MHz satellite line excitation temperatures show that the gas is generally not in LTE. For a selection of sightlines, we compare our OH features to associated (on-sky and in velocity) Hi cold gas components (CNM) identified by Nguyen et al. (2019, ApJ, 880, 141) and find no strong correlations. We speculate that this may indicate an effective decoupling of the molecular gas from the CNM once it accumulates.
{"title":"GNOMES II: Analysis of the Galactic diffuse molecular ISM in all four ground state hydroxyl transitions using Amoeba","authors":"Anita Petzler, J. Dawson, Hiep Nguyen, C. Heiles, M. Wardle, M.-Y. Lee, C. Murray, K. Thompson, S. Stanimirović","doi":"10.1017/pasa.2023.8","DOIUrl":"https://doi.org/10.1017/pasa.2023.8","url":null,"abstract":"Abstract We present observations of the four \u0000$^2 Pi _{3/2},J=3/2$\u0000 ground-rotational state transitions of the hydroxyl molecule (OH) along 107 lines of sight both in and out of the Galactic plane: 92 sets of observations from the Arecibo telescope and 15 sets of observations from the Australia Telescope Compact Array (ATCA). Our Arecibo observations included off-source pointings, allowing us to measure excitation temperature ( \u0000$T_{rm ex}$\u0000 ) and optical depth, while our ATCA observations give optical depth only. We perform Gaussian decomposition using the Automated Molecular Excitation Bayesian line-fitting Algorithm ‘Amoeba’ (Petzler, Dawson, & Wardle 2021, ApJ, 923, 261) fitting all four transitions simultaneously with shared centroid velocity and width. We identify 109 features across 38 sightlines (including 58 detections along 27 sightlines with excitation temperature measurements). While the main lines at 1665 and 1667 MHz tend to have similar excitation temperatures (median \u0000$|Delta T_{rm ex}({rm main})|=0.6,$\u0000 K, 84% show \u0000$|Delta T_{rm ex}({rm main})|<2,$\u0000 K), large differences in the 1612 and 1720 MHz satellite line excitation temperatures show that the gas is generally not in LTE. For a selection of sightlines, we compare our OH features to associated (on-sky and in velocity) Hi cold gas components (CNM) identified by Nguyen et al. (2019, ApJ, 880, 141) and find no strong correlations. We speculate that this may indicate an effective decoupling of the molecular gas from the CNM once it accumulates.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":"154 1","pages":""},"PeriodicalIF":6.3,"publicationDate":"2023-02-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74812003","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
P. Kummamuru, G. M. Calv'es, G. Cimò, S. Pogrebenko, T. M. Bocanegra-Baham'on, D. Duev, M. Said, J. Edwards, M. Ma, J. Quick, A. Neidhardt, P. Vicente, R. Haas, J. Kallunki, 1. G. Maccaferri, G. Colucci, W. J. Yang, L. Hao, S. Weston, M. Kharinov, A. Mikhailov, T. Jung
Abstract The radio signal transmitted by the Mars Express (MEX) spacecraft was observed regularly between the years 2013–2020 at X-band (8.42 GHz) using the European Very Long Baseline Interferometry (EVN) network and University of Tasmania’s telescopes. We present a method to describe the solar wind parameters by quantifying the effects of plasma on our radio signal. In doing so, we identify all the uncompensated effects on the radio signal and see which coronal processes drive them. From a technical standpoint, quantifying the effect of the plasma on the radio signal helps phase referencing for precision spacecraft tracking. The phase fluctuation of the signal was determined for Mars’ orbit for solar elongation angles from 0 to 180 deg. The calculated phase residuals allow determination of the phase power spectrum. The total electron content of the solar plasma along the line of sight is calculated by removing effects from mechanical and ionospheric noises. The spectral index was determined as $-2.43 pm 0.11$ which is in agreement with Kolmogorov’s turbulence. The theoretical models are consistent with observations at lower solar elongations however at higher solar elongation ( $>$ 160 deg) we see the observed values to be higher. This can be caused when the uplink and downlink signals are positively correlated as a result of passing through identical plasma sheets.
{"title":"A monitoring campaign (2013–2020) of ESA’s Mars Express to study interplanetary plasma scintillation","authors":"P. Kummamuru, G. M. Calv'es, G. Cimò, S. Pogrebenko, T. M. Bocanegra-Baham'on, D. Duev, M. Said, J. Edwards, M. Ma, J. Quick, A. Neidhardt, P. Vicente, R. Haas, J. Kallunki, 1. G. Maccaferri, G. Colucci, W. J. Yang, L. Hao, S. Weston, M. Kharinov, A. Mikhailov, T. Jung","doi":"10.1017/pasa.2023.12","DOIUrl":"https://doi.org/10.1017/pasa.2023.12","url":null,"abstract":"Abstract The radio signal transmitted by the Mars Express (MEX) spacecraft was observed regularly between the years 2013–2020 at X-band (8.42 GHz) using the European Very Long Baseline Interferometry (EVN) network and University of Tasmania’s telescopes. We present a method to describe the solar wind parameters by quantifying the effects of plasma on our radio signal. In doing so, we identify all the uncompensated effects on the radio signal and see which coronal processes drive them. From a technical standpoint, quantifying the effect of the plasma on the radio signal helps phase referencing for precision spacecraft tracking. The phase fluctuation of the signal was determined for Mars’ orbit for solar elongation angles from 0 to 180 deg. The calculated phase residuals allow determination of the phase power spectrum. The total electron content of the solar plasma along the line of sight is calculated by removing effects from mechanical and ionospheric noises. The spectral index was determined as \u0000$-2.43 pm 0.11$\u0000 which is in agreement with Kolmogorov’s turbulence. The theoretical models are consistent with observations at lower solar elongations however at higher solar elongation ( \u0000$>$\u0000 160 deg) we see the observed values to be higher. This can be caused when the uplink and downlink signals are positively correlated as a result of passing through identical plasma sheets.","PeriodicalId":20753,"journal":{"name":"Publications of the Astronomical Society of Australia","volume":"26 1","pages":""},"PeriodicalIF":6.3,"publicationDate":"2023-02-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"83266834","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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