We analyzed MUSE observations of 42 local $z<0.1$ type 1 active galactic nucleus (AGN) host galaxies taken from the Palomar-Green quasar sample and the close AGN reference survey. Our goal was to study the relation between the black hole mass ($M_bullet$) and bulge stellar velocity dispersion ($sigma_e$) for type 1 active galaxies. The sample spans black hole masses of $10^{6.0}-10^{9.2},M_odot$, bolometric luminosities of $10^{42.9}-10^{46.0},$erg$,$s$^{-1}$, and Eddington ratios of 0.006-1.2. We avoided AGN emission by extracting the spectra over annular apertures. We modeled the calcium triplet stellar features and measured stellar velocity dispersions of $sigma_* = 60-230,$km$,$s$^{-1}$ for the host galaxies. We find $sigma_*$ values in agreement with previous measurements for local AGN host galaxies, but slightly lower compared with those reported for nearby X-ray-selected type 2 quasars. Using a novel annular aperture correction recipe to estimate $sigma_e$ from $sigma_*$ that considers the bulge morphology and observation beam-smearing, we estimate flux-weighted $sigma_e = 60-250,$km$,$s$^{-1}$. If we consider the bulge type when estimating $M_bullet$, we find no statistical difference between the distributions of AGN hosts and the inactive galaxies on the $M_bullet - sigma_e$ plane for $M_bullet lesssim 10^8,M_odot$. Conversely, if we do not consider the bulge type when computing $M_bullet$, we find that both distributions disagree. We find no correlation between the degree of offset from the $M_bullet - sigma_e$ relation and Eddington ratio for $M_bullet lesssim 10^8,M_odot$. The current statistics preclude firm conclusions from being drawn for the high-mass range. We argue these observations support notions that a significant fraction of the local type 1 AGNs and quasars have undermassive black holes compared with their host galaxy bulge properties.
{"title":"The $M_bullet$-$σ_e$ relation for local type 1 AGNs and quasars","authors":"J. Molina, L. C. Ho, K. K. Knudsen","doi":"arxiv-2409.08893","DOIUrl":"https://doi.org/arxiv-2409.08893","url":null,"abstract":"We analyzed MUSE observations of 42 local $z<0.1$ type 1 active galactic\u0000nucleus (AGN) host galaxies taken from the Palomar-Green quasar sample and the\u0000close AGN reference survey. Our goal was to study the relation between the\u0000black hole mass ($M_bullet$) and bulge stellar velocity dispersion\u0000($sigma_e$) for type 1 active galaxies. The sample spans black hole masses of\u0000$10^{6.0}-10^{9.2},M_odot$, bolometric luminosities of\u0000$10^{42.9}-10^{46.0},$erg$,$s$^{-1}$, and Eddington ratios of 0.006-1.2. We\u0000avoided AGN emission by extracting the spectra over annular apertures. We\u0000modeled the calcium triplet stellar features and measured stellar velocity\u0000dispersions of $sigma_* = 60-230,$km$,$s$^{-1}$ for the host galaxies. We\u0000find $sigma_*$ values in agreement with previous measurements for local AGN\u0000host galaxies, but slightly lower compared with those reported for nearby\u0000X-ray-selected type 2 quasars. Using a novel annular aperture correction recipe\u0000to estimate $sigma_e$ from $sigma_*$ that considers the bulge morphology and\u0000observation beam-smearing, we estimate flux-weighted $sigma_e =\u000060-250,$km$,$s$^{-1}$. If we consider the bulge type when estimating\u0000$M_bullet$, we find no statistical difference between the distributions of AGN\u0000hosts and the inactive galaxies on the $M_bullet - sigma_e$ plane for\u0000$M_bullet lesssim 10^8,M_odot$. Conversely, if we do not consider the bulge\u0000type when computing $M_bullet$, we find that both distributions disagree. We\u0000find no correlation between the degree of offset from the $M_bullet -\u0000sigma_e$ relation and Eddington ratio for $M_bullet lesssim 10^8,M_odot$.\u0000The current statistics preclude firm conclusions from being drawn for the\u0000high-mass range. We argue these observations support notions that a significant\u0000fraction of the local type 1 AGNs and quasars have undermassive black holes\u0000compared with their host galaxy bulge properties.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"28 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267385","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Callum J. O'Kane, Ulrike Kuchner, Meghan E. Gray, Alfonso Aragón-Salamanca
Galaxy properties are known to be affected by their environment. This is well established for the extremes of the density scales, between the high-density cluster environment and the low-density field. It is however not fully understood how the intermediate-density regime of cosmic web filaments affects galaxy evolution. We investigate this environmental effect using a mass complete sample of 23,441 galaxies in the Sloan Digital Sky Survey DR8 Main Galaxy Sample (${M}_{text{Stellar}} > 10^{9.91} text{M}_{odot}$). We define 6 environments, probing different density regimes and representing unique stages in the structure formation process, comparing the differences in star formation activity and morphology between them. We find that galaxies in filaments tend to be less star forming and favour more early-type morphologies than those in the field. These differences persist when considering stellar mass-matched samples, suggesting that this is a consequence of the environment. We further investigate whether these trends are a result of the large scale or local environment through constructing samples matched both in stellar mass and local galaxy density. We find that when also matching in local galaxy density, the differences observed between the filament and field population vanishes, concluding that the environmental effect of filaments can be entirely parameterised by a local galaxy density index. We find that differences can still be seen in comparisons with the interiors of clusters, suggesting these are unique environments which can impart additional physical processes not characterised by local galaxy density.
{"title":"The effect of cosmic web filaments on galaxy evolution","authors":"Callum J. O'Kane, Ulrike Kuchner, Meghan E. Gray, Alfonso Aragón-Salamanca","doi":"arxiv-2409.09028","DOIUrl":"https://doi.org/arxiv-2409.09028","url":null,"abstract":"Galaxy properties are known to be affected by their environment. This is well\u0000established for the extremes of the density scales, between the high-density\u0000cluster environment and the low-density field. It is however not fully\u0000understood how the intermediate-density regime of cosmic web filaments affects\u0000galaxy evolution. We investigate this environmental effect using a mass\u0000complete sample of 23,441 galaxies in the Sloan Digital Sky Survey DR8 Main\u0000Galaxy Sample (${M}_{text{Stellar}} > 10^{9.91} text{M}_{odot}$). We define\u00006 environments, probing different density regimes and representing unique\u0000stages in the structure formation process, comparing the differences in star\u0000formation activity and morphology between them. We find that galaxies in\u0000filaments tend to be less star forming and favour more early-type morphologies\u0000than those in the field. These differences persist when considering stellar\u0000mass-matched samples, suggesting that this is a consequence of the environment.\u0000We further investigate whether these trends are a result of the large scale or\u0000local environment through constructing samples matched both in stellar mass and\u0000local galaxy density. We find that when also matching in local galaxy density,\u0000the differences observed between the filament and field population vanishes,\u0000concluding that the environmental effect of filaments can be entirely\u0000parameterised by a local galaxy density index. We find that differences can\u0000still be seen in comparisons with the interiors of clusters, suggesting these\u0000are unique environments which can impart additional physical processes not\u0000characterised by local galaxy density.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"55 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267384","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
We present 0$.!!^{primeprime}{22}$-resolution CO(2$-$1) observations of the circumnuclear gas disk in the local compact galaxy NGC 384 with the Atacama Large Millimeter/submillimeter Array (ALMA). While the majority of the disk displays regular rotation with projected velocities rising to $370$ km s$^{-1}$, the inner $sim$0farcs{5} exhibits a kinematic twist. We develop warped disk gas-dynamical models to account for this twist, fit those models to the ALMA data cube, and find a stellar mass-to-light ratio in the $H$-band of mlabstract and a supermassive black hole (BH) mass ($M_{mathrm{BH}}$) of $M_{mathrm{BH}}$ $= (7.26^{+0.43}_{-0.48}$ [$1sigma$ statistical] $^{+0.55}_{-1.00}$ [systematic])$times 10^8$ $M_odot$. In contrast to most previous dynamical $M_{mathrm{BH}}$ measurements in local compact galaxies, which typically found over-massive BHs compared to the local BH mass$-$bulge luminosity and BH mass$-$bulge mass relations, NGC 384 lies within the scatter of those scaling relations. NGC 384 and other local compact galaxies are likely relics of $zsim2$ red nuggets, and over-massive BHs in these relics indicate BH growth may conclude before the host galaxy stars have finished assembly. Our NGC 384 results may challenge this evolutionary picture, suggesting there may be increased scatter in the scaling relations than previously thought. However, this scatter could be inflated by systematic differences between stellar- and gas-dynamical measurement methods, motivating direct comparisons between the methods for NGC 384 and the other compact galaxies in the sample.
{"title":"Modeling ALMA Observations of the Warped Molecular Gas Disk in the Red Nugget Relic Galaxy NGC 384","authors":"Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho","doi":"arxiv-2409.08812","DOIUrl":"https://doi.org/arxiv-2409.08812","url":null,"abstract":"We present 0$.!!^{primeprime}{22}$-resolution CO(2$-$1) observations of\u0000the circumnuclear gas disk in the local compact galaxy NGC 384 with the Atacama\u0000Large Millimeter/submillimeter Array (ALMA). While the majority of the disk\u0000displays regular rotation with projected velocities rising to $370$ km\u0000s$^{-1}$, the inner $sim$0farcs{5} exhibits a kinematic twist. We develop\u0000warped disk gas-dynamical models to account for this twist, fit those models to\u0000the ALMA data cube, and find a stellar mass-to-light ratio in the $H$-band of\u0000mlabstract and a supermassive black hole (BH) mass ($M_{mathrm{BH}}$) of\u0000$M_{mathrm{BH}}$ $= (7.26^{+0.43}_{-0.48}$ [$1sigma$ statistical]\u0000$^{+0.55}_{-1.00}$ [systematic])$times 10^8$ $M_odot$. In contrast to most\u0000previous dynamical $M_{mathrm{BH}}$ measurements in local compact galaxies,\u0000which typically found over-massive BHs compared to the local BH mass$-$bulge\u0000luminosity and BH mass$-$bulge mass relations, NGC 384 lies within the scatter\u0000of those scaling relations. NGC 384 and other local compact galaxies are likely\u0000relics of $zsim2$ red nuggets, and over-massive BHs in these relics indicate\u0000BH growth may conclude before the host galaxy stars have finished assembly. Our\u0000NGC 384 results may challenge this evolutionary picture, suggesting there may\u0000be increased scatter in the scaling relations than previously thought. However,\u0000this scatter could be inflated by systematic differences between stellar- and\u0000gas-dynamical measurement methods, motivating direct comparisons between the\u0000methods for NGC 384 and the other compact galaxies in the sample.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"77 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142269539","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Billy Gamache, Laurent Drissen, Carmelle Robert, Mykola Posternak
We present preliminary results of a detailed 3D study of supernova remnants in the nearby spiral M51 using data from the SIGNALS survey obtained with the imaging Fourier transform spectrometer SITELLE at the Canada-France-Hawaii telescope (CFHT). Data cubes covering the entire galaxy were gathered in three spectral ranges: SN3 (647-685 nm, R = 5000), SN2 (482-513 nm, R = 600) and SN1 (363-386 nm, R = 1000). The spectral resolution of the SN3 cube allows a precise, spatially resolved measurement of the velocity dispersion of each object. While most of the SNRs were known from previous surveys based on imagery and long-slit spectroscopy, we now provide 2D line flux and kinematic maps for all of them and found 20 new candidates. Most of the SNRs show velocity dispersions ($sigma$) in the range 30-80 km/s, which is typical for middle-aged SNRs. Finally, we compare the properties of SNRs with those of thousands of HII regions included in the same dataset.
{"title":"Characterization of M51 supernova remnants with the imaging spectrometer SITELLE","authors":"Billy Gamache, Laurent Drissen, Carmelle Robert, Mykola Posternak","doi":"arxiv-2409.08888","DOIUrl":"https://doi.org/arxiv-2409.08888","url":null,"abstract":"We present preliminary results of a detailed 3D study of supernova remnants\u0000in the nearby spiral M51 using data from the SIGNALS survey obtained with the\u0000imaging Fourier transform spectrometer SITELLE at the Canada-France-Hawaii\u0000telescope (CFHT). Data cubes covering the entire galaxy were gathered in three\u0000spectral ranges: SN3 (647-685 nm, R = 5000), SN2 (482-513 nm, R = 600) and SN1\u0000(363-386 nm, R = 1000). The spectral resolution of the SN3 cube allows a\u0000precise, spatially resolved measurement of the velocity dispersion of each\u0000object. While most of the SNRs were known from previous surveys based on\u0000imagery and long-slit spectroscopy, we now provide 2D line flux and kinematic\u0000maps for all of them and found 20 new candidates. Most of the SNRs show\u0000velocity dispersions ($sigma$) in the range 30-80 km/s, which is typical for\u0000middle-aged SNRs. Finally, we compare the properties of SNRs with those of\u0000thousands of HII regions included in the same dataset.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"98 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267264","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Vivienne Wild, Natalia Vale Asari, Kate Rowlands, Sara L. Ellison, Ho-Hin Leung, Christy Tremonti
In galaxies with significant ongoing star formation there is an impressively tight correlation between total infrared luminosity (L$_{TIR}$) and H$alpha$ luminosity (L$_{Halpha}$), when H$alpha$ is properly corrected for stellar absorption and dust attenuation. This long-standing result gives confidence that both measurements provide accurate estimates of a galaxy's star formation rate (SFR), despite their differing origins. To test the extent to which this holds in galaxies with lower specific SFR (sSFR=SFR/Mgal, where Mgal is the stellar mass), we combine optical spectroscopy from the Sloan Digital Sky Survey (SDSS) with multi-wavelength (FUV to FIR) photometric observations from the Galaxy And Mass Assembly survey (GAMA). We find that L$_{TIR}$/L$_{Halpha}$increases steadily with decreasing H$alpha$ equivalent width (W$_{Halpha}$, a proxy for sSFR), indicating that both luminosities cannot provide a valid measurement of SFR in galaxies below the canonical star-forming sequence. For both `retired galaxies' and `post-starburst galaxies', L$_{TIR}$/L$_{Halpha}$ can be up to a factor of 30 larger than for star-forming galaxies. The smooth change in L$_{TIR}$/L$_{Halpha}$, irrespective of star formation history, ionisation or heating source, dust temperature or other properties, suggests that the value of L$_{TIR}$/L$_{Halpha}$ is given by the balance between star-forming regions and ambient interstellar medium contributing to both L$_{TIR}$ and L$_{Halpha}$. While L$_{Halpha}$ can only be used to estimate the SFR for galaxies with W$_{Halpha}$ > 3A (sSFR $gtrsim 10^{-11.5}$/yr), we argue that the mid- and far-infrared can only be used to estimate the SFR of galaxies on the star-forming sequence, and in particular only for galaxies with W$_{Halpha}$ >10 A (sSFR $gtrsim 10^{-10.5}$/yr). We find no evidence for dust obscured star-formation in post-starburst galaxies.
{"title":"The infrared luminosity of retired and post-starburst galaxies: A cautionary tale for star formation rate measurements","authors":"Vivienne Wild, Natalia Vale Asari, Kate Rowlands, Sara L. Ellison, Ho-Hin Leung, Christy Tremonti","doi":"arxiv-2409.08672","DOIUrl":"https://doi.org/arxiv-2409.08672","url":null,"abstract":"In galaxies with significant ongoing star formation there is an impressively\u0000tight correlation between total infrared luminosity (L$_{TIR}$) and H$alpha$\u0000luminosity (L$_{Halpha}$), when H$alpha$ is properly corrected for stellar\u0000absorption and dust attenuation. This long-standing result gives confidence\u0000that both measurements provide accurate estimates of a galaxy's star formation\u0000rate (SFR), despite their differing origins. To test the extent to which this\u0000holds in galaxies with lower specific SFR (sSFR=SFR/Mgal, where Mgal is the\u0000stellar mass), we combine optical spectroscopy from the Sloan Digital Sky\u0000Survey (SDSS) with multi-wavelength (FUV to FIR) photometric observations from\u0000the Galaxy And Mass Assembly survey (GAMA). We find that\u0000L$_{TIR}$/L$_{Halpha}$increases steadily with decreasing H$alpha$ equivalent\u0000width (W$_{Halpha}$, a proxy for sSFR), indicating that both luminosities\u0000cannot provide a valid measurement of SFR in galaxies below the canonical\u0000star-forming sequence. For both `retired galaxies' and `post-starburst\u0000galaxies', L$_{TIR}$/L$_{Halpha}$ can be up to a factor of 30 larger than for\u0000star-forming galaxies. The smooth change in L$_{TIR}$/L$_{Halpha}$,\u0000irrespective of star formation history, ionisation or heating source, dust\u0000temperature or other properties, suggests that the value of\u0000L$_{TIR}$/L$_{Halpha}$ is given by the balance between star-forming regions\u0000and ambient interstellar medium contributing to both L$_{TIR}$ and\u0000L$_{Halpha}$. While L$_{Halpha}$ can only be used to estimate the SFR for\u0000galaxies with W$_{Halpha}$ > 3A (sSFR $gtrsim 10^{-11.5}$/yr), we argue that\u0000the mid- and far-infrared can only be used to estimate the SFR of galaxies on\u0000the star-forming sequence, and in particular only for galaxies with\u0000W$_{Halpha}$ >10 A (sSFR $gtrsim 10^{-10.5}$/yr). We find no evidence for\u0000dust obscured star-formation in post-starburst galaxies.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"49 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267387","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Ruizheng Jiang, Gang Zhao, Haining Li, Qianfan Xing
The most metal-poor stars record the earliest metal enrichment triggered by Population III stars. By comparing observed abundance patterns with theoretical yields of metal-free stars, physical properties of their first star progenitors can be inferred, including zero-age main-sequence mass and explosion energy. In this work, the initial mass distribution (IMF) of first stars is obtained from the largest analysis to date of 406 very metal-poor stars with the newest LAMOST/Subaru high-resolution spectroscopic observations. However, the mass distribution fails to be consistent with the Salpeter IMF, which is also reported by previous studies. Here we modify the standard power-law function with explodability theory. The mass distribution of Population III stars could be well explained by ensuring the initial metal enrichment to originate from successful supernova explosions. Based on the modified power-law function, we suggest an extremely top-heavy or nearly flat initial mass function with a large explosion energy exponent. This indicates that supernova explodability should be considered in the earliest metal enrichment process in the Universe.
{"title":"A Modified Initial Mass Function of the First Stars with Explodability Theory under Different Enrichment Scenarios","authors":"Ruizheng Jiang, Gang Zhao, Haining Li, Qianfan Xing","doi":"arxiv-2409.08659","DOIUrl":"https://doi.org/arxiv-2409.08659","url":null,"abstract":"The most metal-poor stars record the earliest metal enrichment triggered by\u0000Population III stars. By comparing observed abundance patterns with theoretical\u0000yields of metal-free stars, physical properties of their first star progenitors\u0000can be inferred, including zero-age main-sequence mass and explosion energy. In\u0000this work, the initial mass distribution (IMF) of first stars is obtained from\u0000the largest analysis to date of 406 very metal-poor stars with the newest\u0000LAMOST/Subaru high-resolution spectroscopic observations. However, the mass\u0000distribution fails to be consistent with the Salpeter IMF, which is also\u0000reported by previous studies. Here we modify the standard power-law function\u0000with explodability theory. The mass distribution of Population III stars could\u0000be well explained by ensuring the initial metal enrichment to originate from\u0000successful supernova explosions. Based on the modified power-law function, we\u0000suggest an extremely top-heavy or nearly flat initial mass function with a\u0000large explosion energy exponent. This indicates that supernova explodability\u0000should be considered in the earliest metal enrichment process in the Universe.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"197 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267386","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry
We present the CO(1-0) maps of 28 infrared-bright galaxies from the Great Observatories All-Sky Luminous Infrared Galaxy Survey (GOALS) taken with the Combined Array for Research in Millimeter Astronomy (CARMA). We detect 100GHz continuum in 16 of 28 galaxies, which trace both active galactic nuclei (AGNs) and compact star-forming cores. The GOALS galaxies show a variety of molecular gas morphologies, though in the majority of cases, the average velocity fields show a gradient consistent with rotation. We fit the full continuum SEDs of each of the source using either MAGPHYS or SED3FIT (if there are signs of an AGN) to derive the total stellar mass, dust mass, and star formation rates of each object. We adopt a value determined from luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs) of $alpha_{rm CO}=1.5^{+1.3}_{-0.8}~M_odot$ (K km s$^{-1}$ pc$^2)^{-1}$, which leads to more physical values for $f_{rm mol}$ and the gas-to-dust ratio. Mergers tend to have the highest gas-to-dust ratios. We assume the cospatiality of the molecular gas and star formation, and plot the sample on the Schmidt-Kennicutt relation, we find that they preferentially lie above the line set by normal star-forming galaxies. This hyper-efficiency is likely due to the increased turbulence in these systems, which decreases the freefall time compared to star-forming galaxies, leading to "enhanced" star formation efficiency. Line wings are present in a non-negligible subsample (11/28) of the CARMA GOALS sources and are likely due to outflows driven by AGNs or star formation, gas inflows, or additional decoupled gas components.
{"title":"Characterizing the Molecular Gas in Infrared Bright Galaxies with CARMA","authors":"Katherine Alatalo, Andreea O. Petric, Lauranne Lanz, Kate Rowlands, Vivian U, Kirsten L. Larson, Lee Armus, Loreto Barcos-Muñoz, Aaron S. Evans, Jin Koda, Yuanze Luo, Anne M. Medling, Kristina E. Nyland, Justin A. Otter, Pallavi Patil, Fernando Peñaloza, Diane Salim, David B. Sanders, Elizaveta Sazonova, Maya Skarbinski, Yiqing Song, Ezequiel Treister, C. Meg Urry","doi":"arxiv-2409.09116","DOIUrl":"https://doi.org/arxiv-2409.09116","url":null,"abstract":"We present the CO(1-0) maps of 28 infrared-bright galaxies from the Great\u0000Observatories All-Sky Luminous Infrared Galaxy Survey (GOALS) taken with the\u0000Combined Array for Research in Millimeter Astronomy (CARMA). We detect 100GHz\u0000continuum in 16 of 28 galaxies, which trace both active galactic nuclei (AGNs)\u0000and compact star-forming cores. The GOALS galaxies show a variety of molecular\u0000gas morphologies, though in the majority of cases, the average velocity fields\u0000show a gradient consistent with rotation. We fit the full continuum SEDs of\u0000each of the source using either MAGPHYS or SED3FIT (if there are signs of an\u0000AGN) to derive the total stellar mass, dust mass, and star formation rates of\u0000each object. We adopt a value determined from luminous and ultraluminous\u0000infrared galaxies (LIRGs and ULIRGs) of $alpha_{rm\u0000CO}=1.5^{+1.3}_{-0.8}~M_odot$ (K km s$^{-1}$ pc$^2)^{-1}$, which leads to more\u0000physical values for $f_{rm mol}$ and the gas-to-dust ratio. Mergers tend to\u0000have the highest gas-to-dust ratios. We assume the cospatiality of the\u0000molecular gas and star formation, and plot the sample on the Schmidt-Kennicutt\u0000relation, we find that they preferentially lie above the line set by normal\u0000star-forming galaxies. This hyper-efficiency is likely due to the increased\u0000turbulence in these systems, which decreases the freefall time compared to\u0000star-forming galaxies, leading to \"enhanced\" star formation efficiency. Line\u0000wings are present in a non-negligible subsample (11/28) of the CARMA GOALS\u0000sources and are likely due to outflows driven by AGNs or star formation, gas\u0000inflows, or additional decoupled gas components.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"28 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267260","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Eric P. Andersson, Martin P. Rey, Andrew Pontzen, Corentin Cadiou, Oscar Agertz, Justin I. Read, Nicolas F. Martin
Interpretation of data from faint dwarf galaxies is made challenging by observations limited to only the brightest stars. We present a major improvement to tackle this challenge by undertaking zoomed cosmological simulations that resolve the evolution of all individual stars more massive than $0.5,{rm M}_{odot}$, thereby explicitly tracking all observable stars for the Hubble time. For the first time, we predict observable color-magnitude diagrams and the spatial distribution of $approx 100,000$ stars within four faint ($M_{star} approx 10^5 , ,{rm M}_{odot}$) dwarf galaxies directly from their cosmological initial conditions. In all cases, simulations predict complex light profiles with multiple components, implying that typical observational measures of structural parameters can make total V-band magnitudes appear up to 0.5 mag dimmer compared to estimates from simulations. Furthermore, when only small ($lessapprox100$) numbers of stars are observable, shot noise from realizations of the color-magnitude diagram introduces uncertainties comparable to the population scatter in, e.g., total magnitude, half-light radius, and mean iron abundance measurements. Estimating these uncertainties with fully self-consistent mass growth, star formation and chemical enrichment histories paves the way for more robust interpretation of dwarf galaxy data.
{"title":"EDGE-INFERNO: Simulating every observable star in faint dwarf galaxies and their consequences for resolved-star photometric surveys","authors":"Eric P. Andersson, Martin P. Rey, Andrew Pontzen, Corentin Cadiou, Oscar Agertz, Justin I. Read, Nicolas F. Martin","doi":"arxiv-2409.08073","DOIUrl":"https://doi.org/arxiv-2409.08073","url":null,"abstract":"Interpretation of data from faint dwarf galaxies is made challenging by\u0000observations limited to only the brightest stars. We present a major\u0000improvement to tackle this challenge by undertaking zoomed cosmological\u0000simulations that resolve the evolution of all individual stars more massive\u0000than $0.5,{rm M}_{odot}$, thereby explicitly tracking all observable stars\u0000for the Hubble time. For the first time, we predict observable color-magnitude\u0000diagrams and the spatial distribution of $approx 100,000$ stars within four\u0000faint ($M_{star} approx 10^5 , ,{rm M}_{odot}$) dwarf galaxies directly\u0000from their cosmological initial conditions. In all cases, simulations predict\u0000complex light profiles with multiple components, implying that typical\u0000observational measures of structural parameters can make total V-band\u0000magnitudes appear up to 0.5 mag dimmer compared to estimates from simulations.\u0000Furthermore, when only small ($lessapprox100$) numbers of stars are\u0000observable, shot noise from realizations of the color-magnitude diagram\u0000introduces uncertainties comparable to the population scatter in, e.g., total\u0000magnitude, half-light radius, and mean iron abundance measurements. Estimating\u0000these uncertainties with fully self-consistent mass growth, star formation and\u0000chemical enrichment histories paves the way for more robust interpretation of\u0000dwarf galaxy data.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"5 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142195361","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke J. Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais
We measure the absolute proper motion of Andromeda III using ACS/WFC and WFPC2 exposures spanning an unprecedented 22-year time baseline. The WFPC2 exposures have been processed using a deep-learning centering procedure recently developed as well as an improved astrometric calibration of the camera. The absolute proper motion zero point is given by 98 galaxies and 16 Gaia EDR3 stars. The resulting proper motion is $(mu_{alpha} , mu_{delta}) = (-10.5pm12.5, 47.5pm12.5)~mu$as yr$^{-1}$. We perform an orbit analysis of And III using two estimates of M31's mass and proper motion. We find that And III's orbit is consistent with dynamical membership to the Great Plane of Andromeda system of satellites although with some looser alignment compared to the previous two satellites NGC 147 and NGC 185. And III is bound to M31 if M31's mass is $M_{mathrm{vir}}geq 1.5times10^{12},M_{odot}$.
{"title":"HST Proper Motion of Andromeda III: Another Satellite Co-orbiting The M31 Satellite Plane","authors":"Dana I. Casetti-Dinescu, Marcel S. Pawlowski, Terrence M. Girard, Kosuke J. Kanehisa, Alexander Petroski, Max Martone, Vera Kozhurina-Platais, Imants Platais","doi":"arxiv-2409.08252","DOIUrl":"https://doi.org/arxiv-2409.08252","url":null,"abstract":"We measure the absolute proper motion of Andromeda III using ACS/WFC and\u0000WFPC2 exposures spanning an unprecedented 22-year time baseline. The WFPC2\u0000exposures have been processed using a deep-learning centering procedure\u0000recently developed as well as an improved astrometric calibration of the\u0000camera. The absolute proper motion zero point is given by 98 galaxies and 16\u0000Gaia EDR3 stars. The resulting proper motion is $(mu_{alpha} , mu_{delta}) =\u0000(-10.5pm12.5, 47.5pm12.5)~mu$as yr$^{-1}$. We perform an orbit analysis of\u0000And III using two estimates of M31's mass and proper motion. We find that And\u0000III's orbit is consistent with dynamical membership to the Great Plane of\u0000Andromeda system of satellites although with some looser alignment compared to\u0000the previous two satellites NGC 147 and NGC 185. And III is bound to M31 if\u0000M31's mass is $M_{mathrm{vir}}geq 1.5times10^{12},M_{odot}$.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"87 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142195332","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Grayson C. Petter, Ryan C. Hickox, Nickolas Kokron, Michael A. Strauss, Jahmour J. Givans, Yoshiki Toba, Cassandra Starr Henderson
Active galactic nuclei (AGN) are the signposts of black hole growth, and likely play an important role in galaxy evolution. An outstanding question is whether AGN of different spectral types indicate different evolutionary stages in the coevolution of black holes and galaxies. We present the angular correlation function between an AGN sample selected from the Hyper Suprime Camera Subaru Strategic Program (HSC-SSP) optical + Wide-field Infrared Survey Explorer (WISE) mid-IR photometry, and a luminous red galaxy (LRG) sample from HSC-SSP. We investigate AGN clustering strength as a function of their luminosity and spectral features across three independent HSC fields totaling $sim600,{rm deg^{2}}$, for $zin0.6-1.2$ and AGN with $L_{6mu m}>3times10^{44}{rm,erg,s^{-1}}$. There are $sim28,500$ AGN and $sim1.5$ million LRGs in our primary analysis. We determine the inferred average halo mass for the full AGN sample ($M_h approx 10^{12.9}h^{-1}M_odot$), and note that it does not evolve significantly as a function of redshift (over this narrow range) or luminosity. We find that, on average, unobscured AGN ($M_h approx10^{13.3}h^{-1}M_odot$) occupy $sim4.5times$ more massive halos than obscured AGN ($M_h approx10^{12.6}h^{-1}M_odot$), at $5sigma$ statistical significance using 1-D uncertainties, and at $3sigma$ using the full covariance matrix, suggesting a physical difference between unobscured and obscured AGN, beyond the line-of-sight viewing angle. Furthermore, we find evidence for a halo mass dependence on reddening level within the Type I AGN population, which could support the existence of a previously claimed dust-obscured phase in AGN-host galaxy coevolution. However, we also find that even quite small systematic shifts in the redshift distributions of the AGN sample could plausibly explain current and previously observed differences in $M_{h}$.
{"title":"Cross-correlation of Luminous Red Galaxies with ML-selected AGN in HSC-SSP: Unobscured AGN residing in more massive halos","authors":"Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Grayson C. Petter, Ryan C. Hickox, Nickolas Kokron, Michael A. Strauss, Jahmour J. Givans, Yoshiki Toba, Cassandra Starr Henderson","doi":"arxiv-2409.08314","DOIUrl":"https://doi.org/arxiv-2409.08314","url":null,"abstract":"Active galactic nuclei (AGN) are the signposts of black hole growth, and\u0000likely play an important role in galaxy evolution. An outstanding question is\u0000whether AGN of different spectral types indicate different evolutionary stages\u0000in the coevolution of black holes and galaxies. We present the angular\u0000correlation function between an AGN sample selected from the Hyper Suprime\u0000Camera Subaru Strategic Program (HSC-SSP) optical + Wide-field Infrared Survey\u0000Explorer (WISE) mid-IR photometry, and a luminous red galaxy (LRG) sample from\u0000HSC-SSP. We investigate AGN clustering strength as a function of their\u0000luminosity and spectral features across three independent HSC fields totaling\u0000$sim600,{rm deg^{2}}$, for $zin0.6-1.2$ and AGN with $L_{6mu\u0000m}>3times10^{44}{rm,erg,s^{-1}}$. There are $sim28,500$ AGN and $sim1.5$\u0000million LRGs in our primary analysis. We determine the inferred average halo\u0000mass for the full AGN sample ($M_h approx 10^{12.9}h^{-1}M_odot$), and note\u0000that it does not evolve significantly as a function of redshift (over this\u0000narrow range) or luminosity. We find that, on average, unobscured AGN ($M_h\u0000approx10^{13.3}h^{-1}M_odot$) occupy $sim4.5times$ more massive halos than\u0000obscured AGN ($M_h approx10^{12.6}h^{-1}M_odot$), at $5sigma$ statistical\u0000significance using 1-D uncertainties, and at $3sigma$ using the full\u0000covariance matrix, suggesting a physical difference between unobscured and\u0000obscured AGN, beyond the line-of-sight viewing angle. Furthermore, we find\u0000evidence for a halo mass dependence on reddening level within the Type I AGN\u0000population, which could support the existence of a previously claimed\u0000dust-obscured phase in AGN-host galaxy coevolution. However, we also find that\u0000even quite small systematic shifts in the redshift distributions of the AGN\u0000sample could plausibly explain current and previously observed differences in\u0000$M_{h}$.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"52 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267389","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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