Cloud-cloud collisions in splash bridges produced in gas-rich disk galaxy collisions offer a brief but interesting environment to study the effects of shocks and turbulence on star formation rates in the diffuse IGM, far from the significant feedback effects of massive star formation and AGN. Expanding on our earlier work, we describe simulated collisions between counter-rotating disk galaxies of relatively similar mass, focusing on the thermal and kinematic effects of relative inclination and disk offset at the closest approach. This includes essential heating and cooling signatures, which go some way towards explaining the luminous power in H$_2$ and [CII] emission in the Taffy bridge, as well as providing a partial explanation of the turbulent nature of the recently observed compact CO-emitting clouds observed in Taffy by ALMA. The models show counter-rotating disk collisions result in swirling, shearing kinematics for the gas in much of the post-collision bridge. Gas with little specific angular momentum due to collisions between counter-rotating streams accumulates near the center of mass. The disturbances and mixing in the bridge drive continuing cloud collisions, differential shock heating, and cooling throughout. A wide range of relative gas phases and line-of-sight velocity distributions are found in the bridges, depending sensitively on initial disk orientations and the resulting variety of cloud collision histories. Most cloud collisions can occur promptly or persist for quite a long duration. Cold and hot phases can largely overlap throughout the bridge or can be separated into different parts of the bridge.
在富含气体的盘状星系碰撞中产生的飞溅桥中的云云碰撞，为研究冲击和湍流对弥漫IGM中恒星形成率的影响提供了一个短暂而有趣的环境，因为它远离大质量恒星形成和AGN的重要反馈效应。在我们早期工作的基础上，我们描述了质量相对相似的逆旋转盘星系之间的模拟碰撞，重点研究了最近接近时相对倾角和盘偏移的热效应和运动学效应。这包括基本的加热和冷却特征，这些特征在一定程度上解释了塔菲桥中 H$_2$ 和 [CII] 辐射的发光功率，并部分解释了最近 ALMA 在塔菲桥观测到的紧凑 CO 发射云的湍流性质。模型显示，反向旋转的圆盘碰撞导致碰撞后桥中大部分气体的漩涡和剪切运动。由于反向旋转气流之间的碰撞，特定角动量很小的气体聚集在质量中心附近。桥中的扰动和混合推动了持续的云碰撞、差震加热和冷却。云桥中的相对气体相位和视线速度分布范围很广，这取决于磁盘的初始方位和由此产生的各种云碰撞历史。大多数云碰撞可能很快发生，也可能持续很长时间。冷相和热相在整个云桥中可以基本重叠，也可以分隔在云桥的不同部分。
{"title":"The generation of a multi-phase medium in \"Splash\" bridge systems: Towards an understanding of star formation suppression in turbulent galaxy systems","authors":"Travis Yeager, Curtis Struck, Phil Appleton","doi":"arxiv-2409.11707","DOIUrl":"https://doi.org/arxiv-2409.11707","url":null,"abstract":"Cloud-cloud collisions in splash bridges produced in gas-rich disk galaxy\u0000collisions offer a brief but interesting environment to study the effects of\u0000shocks and turbulence on star formation rates in the diffuse IGM, far from the\u0000significant feedback effects of massive star formation and AGN. Expanding on\u0000our earlier work, we describe simulated collisions between counter-rotating\u0000disk galaxies of relatively similar mass, focusing on the thermal and kinematic\u0000effects of relative inclination and disk offset at the closest approach. This\u0000includes essential heating and cooling signatures, which go some way towards\u0000explaining the luminous power in H$_2$ and [CII] emission in the Taffy bridge,\u0000as well as providing a partial explanation of the turbulent nature of the\u0000recently observed compact CO-emitting clouds observed in Taffy by ALMA. The\u0000models show counter-rotating disk collisions result in swirling, shearing\u0000kinematics for the gas in much of the post-collision bridge. Gas with little\u0000specific angular momentum due to collisions between counter-rotating streams\u0000accumulates near the center of mass. The disturbances and mixing in the bridge\u0000drive continuing cloud collisions, differential shock heating, and cooling\u0000throughout. A wide range of relative gas phases and line-of-sight velocity\u0000distributions are found in the bridges, depending sensitively on initial disk\u0000orientations and the resulting variety of cloud collision histories. Most cloud\u0000collisions can occur promptly or persist for quite a long duration. Cold and\u0000hot phases can largely overlap throughout the bridge or can be separated into\u0000different parts of the bridge.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"49 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267099","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}
M. Nonhebel, A. T. Barnes, K. Immer, J. Armijos-Abendaño, J. Bally, C. Battersby, M. G. Burton, N. Butterfield, L. Colzi, P. García, A. Ginsburg, J. D. Henshaw, Y. Hu, I. Jiménez-Serra, R. S. Klessen, F. -H. Liang, S. N. Longmore, X. Lu, S. Martín, F. Nogueras-Lara, M. A. Petkova, J. E. Pineda, V. M. Rivilla, Á. Sánchez-Monge, M. G. Santa-Maria, H. A. Smith, Y. Sofue, M. C. Sormani, V. Tolls, D. L. Walker, Q. D. Wang, G. M. Williams, F. -W. Xu
The Milky Way's Central Molecular Zone (CMZ) differs dramatically from our local solar neighbourhood, both in the extreme interstellar medium conditions it exhibits (e.g. high gas, stellar, and feedback density) and in the strong dynamics at play (e.g. due to shear and gas influx along the bar). Consequently, it is likely that there are large-scale physical structures within the CMZ that cannot form elsewhere in the Milky Way. In this paper, we present new results from the Atacama Large Millimeter/submillimeter Array (ALMA) large programme ACES (ALMA CMZ Exploration Survey) and conduct a multi-wavelength and kinematic analysis to determine the origin of the M0.8$-$0.2 ring, a molecular cloud with a distinct ring-like morphology. We estimate the projected inner and outer radii of the M0.8$-$0.2 ring to be 79" and 154", respectively (3.1 pc and 6.1 pc at an assumed Galactic Centre distance of 8.2 kpc) and calculate a mean gas density $> 10^{4}$ cm$^{-3}$, a mass of $sim$ $10^6$ M$_odot$, and an expansion speed of $sim$ 20 km s$^{-1}$, resulting in a high estimated kinetic energy ($> 10^{51}$ erg) and momentum ($> 10^7$ M$_odot$ km s$^{-1}$). We discuss several possible causes for the existence and expansion of the structure, including stellar feedback and large-scale dynamics. We propose that the most likely cause of the M0.8$-$0.2 ring is a single high-energy hypernova explosion. To viably explain the observed morphology and kinematics, such an explosion would need to have taken place inside a dense, very massive molecular cloud, the remnants of which we now see as the M0.8$-$0.2 ring. In this case, the structure provides an extreme example of how supernovae can affect molecular clouds.
{"title":"Disruption of a massive molecular cloud by a supernova in the Galactic Centre: Initial results from the ACES project","authors":"M. Nonhebel, A. T. Barnes, K. Immer, J. Armijos-Abendaño, J. Bally, C. Battersby, M. G. Burton, N. Butterfield, L. Colzi, P. García, A. Ginsburg, J. D. Henshaw, Y. Hu, I. Jiménez-Serra, R. S. Klessen, F. -H. Liang, S. N. Longmore, X. Lu, S. Martín, F. Nogueras-Lara, M. A. Petkova, J. E. Pineda, V. M. Rivilla, Á. Sánchez-Monge, M. G. Santa-Maria, H. A. Smith, Y. Sofue, M. C. Sormani, V. Tolls, D. L. Walker, Q. D. Wang, G. M. Williams, F. -W. Xu","doi":"arxiv-2409.12185","DOIUrl":"https://doi.org/arxiv-2409.12185","url":null,"abstract":"The Milky Way's Central Molecular Zone (CMZ) differs dramatically from our\u0000local solar neighbourhood, both in the extreme interstellar medium conditions\u0000it exhibits (e.g. high gas, stellar, and feedback density) and in the strong\u0000dynamics at play (e.g. due to shear and gas influx along the bar).\u0000Consequently, it is likely that there are large-scale physical structures\u0000within the CMZ that cannot form elsewhere in the Milky Way. In this paper, we\u0000present new results from the Atacama Large Millimeter/submillimeter Array\u0000(ALMA) large programme ACES (ALMA CMZ Exploration Survey) and conduct a\u0000multi-wavelength and kinematic analysis to determine the origin of the\u0000M0.8$-$0.2 ring, a molecular cloud with a distinct ring-like morphology. We\u0000estimate the projected inner and outer radii of the M0.8$-$0.2 ring to be 79\"\u0000and 154\", respectively (3.1 pc and 6.1 pc at an assumed Galactic Centre\u0000distance of 8.2 kpc) and calculate a mean gas density $> 10^{4}$ cm$^{-3}$, a\u0000mass of $sim$ $10^6$ M$_odot$, and an expansion speed of $sim$ 20 km\u0000s$^{-1}$, resulting in a high estimated kinetic energy ($> 10^{51}$ erg) and\u0000momentum ($> 10^7$ M$_odot$ km s$^{-1}$). We discuss several possible causes\u0000for the existence and expansion of the structure, including stellar feedback\u0000and large-scale dynamics. We propose that the most likely cause of the\u0000M0.8$-$0.2 ring is a single high-energy hypernova explosion. To viably explain\u0000the observed morphology and kinematics, such an explosion would need to have\u0000taken place inside a dense, very massive molecular cloud, the remnants of which\u0000we now see as the M0.8$-$0.2 ring. In this case, the structure provides an\u0000extreme example of how supernovae can affect molecular clouds.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"22 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142269533","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}
Gan Luo, Laura Colzi, Tie Liu, Thomas G. Bisbas, Di Li, Yichen Sun, Ningyu Tang
We present a new constraint on the Galactic $^{12}$C/$^{13}$C gradient with sensitive HCO$^+$ absorption observations against strong continuum sources. The new measurements suffer less from beam dilution, optical depths, and chemical fractionation, allowing us to derive the isotopic ratios precisely. The measured $^{12}$C/$^{13}$C ratio in the Solar neighborhood (66$pm$5) is consistent with those obtained from CH$^+$. Two measurements toward the Galactic Center are 42.2$pm$1.7 and 37.5$pm$6.5. Though the values are a factor of 2$sim$3 higher than those derived from dense gas tracers (e.g., H$_2$CO, complex organic molecules) toward Sagittarius (Sgr) B2 regions, our results are consistent with the absorption measurements from c-C$_3$H$_2$ toward Sgr B2 ($sim$40), and those from CH$^+$ toward Sgr A$^*$ and Sgr B2(N) ($>$30). We calculate a new Galactic $^{12}$C/$^{13}$C gradient of (6.4$pm$1.9)$R_{rm GC}$/kpc+(25.9$pm$10.5), and find an increasing trend of $^{12}$C/$^{13}$C gradient obtained from high-density to low-density gas tracers, suggesting opacity effects and chemical fractionation may have a strong impact on the isotopic ratios observed at high-density regions.
{"title":"A new measurement of the Galactic $^{12}$C/$^{13}$C gradient from sensitive HCO$^+$ absorption observations","authors":"Gan Luo, Laura Colzi, Tie Liu, Thomas G. Bisbas, Di Li, Yichen Sun, Ningyu Tang","doi":"arxiv-2409.11821","DOIUrl":"https://doi.org/arxiv-2409.11821","url":null,"abstract":"We present a new constraint on the Galactic $^{12}$C/$^{13}$C gradient with\u0000sensitive HCO$^+$ absorption observations against strong continuum sources. The\u0000new measurements suffer less from beam dilution, optical depths, and chemical\u0000fractionation, allowing us to derive the isotopic ratios precisely. The\u0000measured $^{12}$C/$^{13}$C ratio in the Solar neighborhood (66$pm$5) is\u0000consistent with those obtained from CH$^+$. Two measurements toward the\u0000Galactic Center are 42.2$pm$1.7 and 37.5$pm$6.5. Though the values are a\u0000factor of 2$sim$3 higher than those derived from dense gas tracers (e.g.,\u0000H$_2$CO, complex organic molecules) toward Sagittarius (Sgr) B2 regions, our\u0000results are consistent with the absorption measurements from c-C$_3$H$_2$\u0000toward Sgr B2 ($sim$40), and those from CH$^+$ toward Sgr A$^*$ and Sgr B2(N)\u0000($>$30). We calculate a new Galactic $^{12}$C/$^{13}$C gradient of\u0000(6.4$pm$1.9)$R_{rm GC}$/kpc+(25.9$pm$10.5), and find an increasing trend of\u0000$^{12}$C/$^{13}$C gradient obtained from high-density to low-density gas\u0000tracers, suggesting opacity effects and chemical fractionation may have a\u0000strong impact on the isotopic ratios observed at high-density regions.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"98 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267101","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}
I. F. van Leeuwen, R. J. Bouwens, P. P. van der Werf, J. A. Hodge, S. Schouws, M. Stefanon, H. S. B. Algera, M. Aravena, L. A. Boogaard, R. A . A. Bowler, E. da Cunha, P. Dayal, R. Decarli, V. Gonzalez, H. Inami, I. de Looze, L. Sommovigo, B. P. Venemans, F. Walter, L. Barrufet, A. Ferrara, L. Graziani, A. P. S. Hygate, P. Oesch, M. Palla, L. Rowland, R. Schneider
We present a new method to determine the star formation rate (SFR) density of the Universe at $z gtrsim 5$ that includes the contribution of dust-obscured star formation. For this purpose, we use a [CII] (158 $mu$m) selected sample of galaxies serendipitously identified in the fields of known $zgtrsim 4.5$ objects to characterize the fraction of obscured SFR. The advantage of a [CII] selection is that our sample is SFR-selected, in contrast to a UV-selection that would be biased towards unobscured star formation. We obtain a sample of 23 [CII] emitters near star-forming (SF) galaxies and QSOs -- three of which we identify for the first time -- using previous literature and archival ALMA data. 18 of these serendipitously identified galaxies have sufficiently deep rest-UV data and are used to characterize the obscured fraction of the star formation in galaxies with SFRs $gtrsim 30 text{M}_{odot} text{yr}^{-1}$. We find that [CII] emitters identified around SF galaxies have $approx$63% of their SFR obscured, while [CII] emitters around QSOs have $approx$93% of their SFR obscured. By forward modeling existing wide-area UV luminosity function (LF) determinations, we derive the intrinsic UV LF using our characterization of the obscured SFR. Integrating the intrinsic LF to $M_{UV}$ = $-$20 we find that the obscured SFRD contributes to $>3%$ and $>10%$ of the total SFRD at $z sim 5$ and $z sim 6$ based on our sample of companions galaxies near SFGs and QSOs, respectively. Our results suggest that dust obscuration is not negligible at $zgtrsim 5$, further underlining the importance of far-IR observations of the $zgtrsim 5$ Universe.
{"title":"Characterizing the contribution of dust-obscured star formation at $z gtrsim$ 5 using 18 serendipitously identified [CII] emitters","authors":"I. F. van Leeuwen, R. J. Bouwens, P. P. van der Werf, J. A. Hodge, S. Schouws, M. Stefanon, H. S. B. Algera, M. Aravena, L. A. Boogaard, R. A . A. Bowler, E. da Cunha, P. Dayal, R. Decarli, V. Gonzalez, H. Inami, I. de Looze, L. Sommovigo, B. P. Venemans, F. Walter, L. Barrufet, A. Ferrara, L. Graziani, A. P. S. Hygate, P. Oesch, M. Palla, L. Rowland, R. Schneider","doi":"arxiv-2409.11463","DOIUrl":"https://doi.org/arxiv-2409.11463","url":null,"abstract":"We present a new method to determine the star formation rate (SFR) density of\u0000the Universe at $z gtrsim 5$ that includes the contribution of dust-obscured\u0000star formation. For this purpose, we use a [CII] (158 $mu$m) selected sample\u0000of galaxies serendipitously identified in the fields of known $zgtrsim 4.5$\u0000objects to characterize the fraction of obscured SFR. The advantage of a [CII]\u0000selection is that our sample is SFR-selected, in contrast to a UV-selection\u0000that would be biased towards unobscured star formation. We obtain a sample of\u000023 [CII] emitters near star-forming (SF) galaxies and QSOs -- three of which we\u0000identify for the first time -- using previous literature and archival ALMA\u0000data. 18 of these serendipitously identified galaxies have sufficiently deep\u0000rest-UV data and are used to characterize the obscured fraction of the star\u0000formation in galaxies with SFRs $gtrsim 30 text{M}_{odot} \u0000text{yr}^{-1}$. We find that [CII] emitters identified around SF galaxies have\u0000$approx$63% of their SFR obscured, while [CII] emitters around QSOs have\u0000$approx$93% of their SFR obscured. By forward modeling existing wide-area UV\u0000luminosity function (LF) determinations, we derive the intrinsic UV LF using\u0000our characterization of the obscured SFR. Integrating the intrinsic LF to\u0000$M_{UV}$ = $-$20 we find that the obscured SFRD contributes to $>3%$ and\u0000$>10%$ of the total SFRD at $z sim 5$ and $z sim 6$ based on our sample of\u0000companions galaxies near SFGs and QSOs, respectively. Our results suggest that\u0000dust obscuration is not negligible at $zgtrsim 5$, further underlining the\u0000importance of far-IR observations of the $zgtrsim 5$ Universe.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"119 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142269536","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}
Lee R. Martin, Andrew W. Blain, Tanio Díaz-Santos, Roberto J. Assef, Chao-Wei Tsai, Hyunsung D. Jun, Peter R. M. Eisenhardt, Jingwen Wu, Andrey Vayner, Román Fernández Aranda
We present observations of mid-J J=4-3 or J=5-4 carbon monoxide (CO) emission lines and continuum emission from a sample of ten of the most luminous log(L/L_solar)~14 Hot Dust-Obscured Galaxies (Hot DOGs) discovered by the Wide-field Infrared Survey Explorer (WISE) with redshifts up to 4.6. We uncover broad spectral lines (FWHM~400 km/s) in these objects, suggesting a turbulent molecular interstellar medium (ISM) may be ubiquitous in Hot DOGs. A halo of molecular gas, extending out to a radius of 5 kpc is observed in W2305-0039, likely supplied by 940 km/s molecular outflows. W0831+0140 is plausibly the host of a merger between at least two galaxies, consistent with observations made using ionized gas. These CO(4-3) observations contrast with previous CO(1-0) studies of the same sources: the CO(4-3) to CO(1-0) luminosity ratios exceed 300 in each source, suggesting that the lowest excited states of CO are underluminous. These findings show that the molecular gas in Hot DOGs is consistently turbulent, plausibly a consequence of AGN feedback, triggered by galactic mergers.
{"title":"CO spectra of the ISM in the Host Galaxies of the Most Luminous WISE-Selected AGNs","authors":"Lee R. Martin, Andrew W. Blain, Tanio Díaz-Santos, Roberto J. Assef, Chao-Wei Tsai, Hyunsung D. Jun, Peter R. M. Eisenhardt, Jingwen Wu, Andrey Vayner, Román Fernández Aranda","doi":"arxiv-2409.11013","DOIUrl":"https://doi.org/arxiv-2409.11013","url":null,"abstract":"We present observations of mid-J J=4-3 or J=5-4 carbon monoxide (CO) emission\u0000lines and continuum emission from a sample of ten of the most luminous\u0000log(L/L_solar)~14 Hot Dust-Obscured Galaxies (Hot DOGs) discovered by the\u0000Wide-field Infrared Survey Explorer (WISE) with redshifts up to 4.6. We uncover\u0000broad spectral lines (FWHM~400 km/s) in these objects, suggesting a turbulent\u0000molecular interstellar medium (ISM) may be ubiquitous in Hot DOGs. A halo of\u0000molecular gas, extending out to a radius of 5 kpc is observed in W2305-0039,\u0000likely supplied by 940 km/s molecular outflows. W0831+0140 is plausibly the\u0000host of a merger between at least two galaxies, consistent with observations\u0000made using ionized gas. These CO(4-3) observations contrast with previous\u0000CO(1-0) studies of the same sources: the CO(4-3) to CO(1-0) luminosity ratios\u0000exceed 300 in each source, suggesting that the lowest excited states of CO are\u0000underluminous. These findings show that the molecular gas in Hot DOGs is\u0000consistently turbulent, plausibly a consequence of AGN feedback, triggered by\u0000galactic mergers.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"57 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267104","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}
Jared Siegel, David Setton, Jenny Greene, Katherine Suess, Katherine Whitaker, Rachel Bezanson, Joel Leja, Lukas Furtak, Sam Cutler, Anna de Graaff, Robert Feldmann, Gourav Khullar, Ivo Labbé, Danilo Marchesini, Tim Miller, Themiya Nanayakkara, Richard Pan, Sedona Price, Helena Treiber, Pieter van Dokkum, Bingjie Wang, John Weaver
We explore the physical properties of five massive quiescent galaxies at $zsim2.5$, revealing the presence of non-negligible dust reservoirs. JWST NIRSpec observations were obtained for each target, finding no significant line emission; multiple star formation tracers independently place upper limits between $0.1-10~M_odot / mathrm{yr}$. Spectral energy distribution modeling with Prospector infers stellar masses between $log_{10}[M / M_odot] sim 10-11$ and stellar mass-weighted ages between $1-2$ Gyr. The inferred mass-weighted effective radii ($r_{eff}sim 0.4-1.4$ kpc) and inner $1$ kpc stellar surface densities ($log_{10}[Sigma / M_odot mathrm{kpc}^2 ]gtrsim 9$) are typical of quiescent galaxies at $z gtrsim 2$. The galaxies display negative color gradients (redder core and bluer outskirts); for one galaxy, this effect results from a dusty core, while for the others it may be evidence of an "inside-out" growth process. Unlike local quiescent galaxies, we identify significant reddening in these typical cosmic noon passive galaxies; all but one require $A_V gtrsim 0.4$. This finding is in qualitative agreement with previous studies but our deep 20-band NIRCam imaging is able to significantly suppress the dust-age degeneracy and confidently determine that these galaxies are reddened. We speculate about the physical effects that may drive the decline in dust content in quiescent galaxies over cosmic time.
{"title":"UNCOVER: Significant Reddening in Cosmic Noon Quiescent Galaxies","authors":"Jared Siegel, David Setton, Jenny Greene, Katherine Suess, Katherine Whitaker, Rachel Bezanson, Joel Leja, Lukas Furtak, Sam Cutler, Anna de Graaff, Robert Feldmann, Gourav Khullar, Ivo Labbé, Danilo Marchesini, Tim Miller, Themiya Nanayakkara, Richard Pan, Sedona Price, Helena Treiber, Pieter van Dokkum, Bingjie Wang, John Weaver","doi":"arxiv-2409.11457","DOIUrl":"https://doi.org/arxiv-2409.11457","url":null,"abstract":"We explore the physical properties of five massive quiescent galaxies at\u0000$zsim2.5$, revealing the presence of non-negligible dust reservoirs. JWST\u0000NIRSpec observations were obtained for each target, finding no significant line\u0000emission; multiple star formation tracers independently place upper limits\u0000between $0.1-10~M_odot / mathrm{yr}$. Spectral energy distribution modeling\u0000with Prospector infers stellar masses between $log_{10}[M / M_odot] sim\u000010-11$ and stellar mass-weighted ages between $1-2$ Gyr. The inferred\u0000mass-weighted effective radii ($r_{eff}sim 0.4-1.4$ kpc) and inner $1$ kpc\u0000stellar surface densities ($log_{10}[Sigma / M_odot mathrm{kpc}^2 ]gtrsim\u00009$) are typical of quiescent galaxies at $z gtrsim 2$. The galaxies display\u0000negative color gradients (redder core and bluer outskirts); for one galaxy,\u0000this effect results from a dusty core, while for the others it may be evidence\u0000of an \"inside-out\" growth process. Unlike local quiescent galaxies, we identify\u0000significant reddening in these typical cosmic noon passive galaxies; all but\u0000one require $A_V gtrsim 0.4$. This finding is in qualitative agreement with\u0000previous studies but our deep 20-band NIRCam imaging is able to significantly\u0000suppress the dust-age degeneracy and confidently determine that these galaxies\u0000are reddened. We speculate about the physical effects that may drive the\u0000decline in dust content in quiescent galaxies over cosmic time.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"28 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267102","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}
N. E. P. Lines, R. A. A. Bowler, N. J. Adams, R. Fisher, R. G. Varadaraj, Y. Nakazato, M. Aravena, R. J. Assef, J. E. Birkin, D. Ceverino, E. da Cunha, F. Cullen, I. De Looze, C. T. Donnan, J. S. Dunlop, A. Ferrara, N. A. Grogin, R. Herrera-Camus, R. Ikeda, A. M. Koekemoer, M. Killi, J. Li, D. J. McLeod, R. J. McLure, I. Mitsuhashi, P. G. Pérez-González, M. Relano, M. Solimano, J. S. Spilker, V. Villanueva, N. Yoshida
We present a spatially resolved analysis of four star-forming galaxies at $z = 4.44-5.64$ using data from the JWST PRIMER and ALMA-CRISTAL surveys to probe the stellar and inter-stellar medium properties on the sub-kpc scale. In the $1-5,mu{rm m}$ JWST NIRCam imaging we find that the galaxies are composed of multiple clumps (between $2$ and $sim 8$) separated by $simeq 5,{rm kpc}$, with comparable morphologies and sizes in the rest-frame UV and optical. Using BAGPIPES to perform pixel-by-pixel SED fitting to the JWST data we show that the SFR ($simeq 25,{rm M}_{odot}/{rm yr}$) and stellar mass (${rm log}_{10}(M_{star}/{rm M}_{odot}) simeq 9.5$) derived from the resolved analysis are in close ($ lesssim 0.3,{rm dex}$) agreement with those obtained by fitting the integrated photometry. In contrast to studies of lower-mass sources, we thus find a reduced impact of outshining of the older (more massive) stellar populations in these normal $z simeq 5$ galaxies. Our JWST analysis recovers bluer rest-frame UV slopes ($beta simeq -2.1$) and younger ages ($simeq 100,{rm Myr}$) than archival values. We find that the dust continuum from ALMA-CRISTAL seen in two of these galaxies correlates, as expected, with regions of redder rest-frame UV slopes and the SED-derived $A_{rm V}$, as well as the peak in the stellar mass map. We compute the resolved IRX-$beta$ relation, showing that the IRX is consistent with the local starburst attenuation curve and further demonstrating the presence of an inhomogeneous dust distribution within the galaxies. A comparison of the CRISTAL sources to those from the FirstLight zoom-in simulation of galaxies with the same $M_{star}$ and SFR reveals similar age and colour gradients, suggesting that major mergers may be important in the formation of clumpy galaxies at this epoch.
{"title":"JWST PRIMER: A lack of outshining in four normal z =4-6 galaxies from the ALMA-CRISTAL Survey","authors":"N. E. P. Lines, R. A. A. Bowler, N. J. Adams, R. Fisher, R. G. Varadaraj, Y. Nakazato, M. Aravena, R. J. Assef, J. E. Birkin, D. Ceverino, E. da Cunha, F. Cullen, I. De Looze, C. T. Donnan, J. S. Dunlop, A. Ferrara, N. A. Grogin, R. Herrera-Camus, R. Ikeda, A. M. Koekemoer, M. Killi, J. Li, D. J. McLeod, R. J. McLure, I. Mitsuhashi, P. G. Pérez-González, M. Relano, M. Solimano, J. S. Spilker, V. Villanueva, N. Yoshida","doi":"arxiv-2409.10963","DOIUrl":"https://doi.org/arxiv-2409.10963","url":null,"abstract":"We present a spatially resolved analysis of four star-forming galaxies at $z\u0000= 4.44-5.64$ using data from the JWST PRIMER and ALMA-CRISTAL surveys to probe\u0000the stellar and inter-stellar medium properties on the sub-kpc scale. In the\u0000$1-5,mu{rm m}$ JWST NIRCam imaging we find that the galaxies are composed of\u0000multiple clumps (between $2$ and $sim 8$) separated by $simeq 5,{rm kpc}$,\u0000with comparable morphologies and sizes in the rest-frame UV and optical. Using\u0000BAGPIPES to perform pixel-by-pixel SED fitting to the JWST data we show that\u0000the SFR ($simeq 25,{rm M}_{odot}/{rm yr}$) and stellar mass (${rm\u0000log}_{10}(M_{star}/{rm M}_{odot}) simeq 9.5$) derived from the resolved\u0000analysis are in close ($ lesssim 0.3,{rm dex}$) agreement with those\u0000obtained by fitting the integrated photometry. In contrast to studies of\u0000lower-mass sources, we thus find a reduced impact of outshining of the older\u0000(more massive) stellar populations in these normal $z simeq 5$ galaxies. Our\u0000JWST analysis recovers bluer rest-frame UV slopes ($beta simeq -2.1$) and\u0000younger ages ($simeq 100,{rm Myr}$) than archival values. We find that the\u0000dust continuum from ALMA-CRISTAL seen in two of these galaxies correlates, as\u0000expected, with regions of redder rest-frame UV slopes and the SED-derived\u0000$A_{rm V}$, as well as the peak in the stellar mass map. We compute the\u0000resolved IRX-$beta$ relation, showing that the IRX is consistent with the\u0000local starburst attenuation curve and further demonstrating the presence of an\u0000inhomogeneous dust distribution within the galaxies. A comparison of the\u0000CRISTAL sources to those from the FirstLight zoom-in simulation of galaxies\u0000with the same $M_{star}$ and SFR reveals similar age and colour gradients,\u0000suggesting that major mergers may be important in the formation of clumpy\u0000galaxies at this epoch.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"316 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267326","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}
We present a new algorithm for identifying superbubbles in HI column density maps of both observed and simulated galaxies that has only a single adjustable parameter. The algorithm includes an automated galaxy-background separation step to focus the analysis on the galactic disk. To test the algorithm, we compare the superbubbles it finds in a simulated galactic disk with the ones it finds in 21cm observations of a similar galactic disk. The sizes and radial distribution of those superbubbles are indeed qualitatively similar. However, superbubbles in the simulated galactic disk have lower central HI column densities. The HI superbubbles in the simulated disk are spatially associated with pockets of hot gas. We conclude that the algorithm is a promising method for systematically identifying and characterizing superbubbles using only HI column density maps that will enable standardized tests of stellar feedback models used in galaxy simulations.
我们提出了一种在观测和模拟星系的 HI 柱密度图中识别超级气泡的新算法，这种算法只有一个可调参数。该算法包括一个自动的星系-背景分离步骤，以便将分析重点放在星系盘上。为了测试该算法，我们将它在模拟星系盘中发现的超级气泡与它在 21 厘米观测类似星系盘时发现的超级气泡进行了比较。这些超级气泡的大小和径向分布在本质上确实相似。然而，模拟星系盘中的超级气泡的中心 HI 柱密度较低。模拟星系盘中的 HI 超级气泡在空间上与热气体袋相关联。我们的结论是，该算法是一种很有前途的方法，它可以只利用HI柱密度图来系统地识别和描述超级气泡，从而对星系模拟中使用的恒星反馈模型进行标准化测试。
{"title":"A New Superbubble Finding Algorithm: Description and Testing","authors":"Brock Wallin, Benjamin D. Wibking, G. Mark Voit","doi":"arxiv-2409.11556","DOIUrl":"https://doi.org/arxiv-2409.11556","url":null,"abstract":"We present a new algorithm for identifying superbubbles in HI column density\u0000maps of both observed and simulated galaxies that has only a single adjustable\u0000parameter. The algorithm includes an automated galaxy-background separation\u0000step to focus the analysis on the galactic disk. To test the algorithm, we\u0000compare the superbubbles it finds in a simulated galactic disk with the ones it\u0000finds in 21cm observations of a similar galactic disk. The sizes and radial\u0000distribution of those superbubbles are indeed qualitatively similar. However,\u0000superbubbles in the simulated galactic disk have lower central HI column\u0000densities. The HI superbubbles in the simulated disk are spatially associated\u0000with pockets of hot gas. We conclude that the algorithm is a promising method\u0000for systematically identifying and characterizing superbubbles using only HI\u0000column density maps that will enable standardized tests of stellar feedback\u0000models used in galaxy simulations.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"52 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267098","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}
A. B. Drake, D. J. B. Smith, M. J. Hardcastle, P. N. Best, R. Kondapally, M. I. Arnaudova, S. Das, S. Shenoy, K. J. Duncan, H. J. A. Röttgering, C. Tasse
We present an analysis of 152,355 radio sources identified in the second data release of the LOFAR Two Metre Sky Survey (LoTSS-DR2) with Sloan Digital Sky Survey (SDSS) spectroscopic redshifts in the range 0.00 < z < 0.57. Using Monte Carlo simulations we determine the reliability of each source exhibiting an excess in radio luminosity relative to that predicted from their Ha emission, and, for a subset of 124,023 sources we combine this measurement with a full BPT analysis. Using these two independent diagnostics we determine the reliability of each source hosting a supermassive black hole of high or low Eddington-scaled accretion rate, and combine the measurements to determine the reliability of sources belonging to each of four physical classes of objects: star forming galaxies (SFGs), radio-quiet active galactic nuclei (RQAGN), and high- or low-excitation radio galaxies (HERGs or emission-line LERGs). The result is a catalogue which enables user-defined samples of radio sources with a reliability threshold suited to their science goal e.g. prioritising purity or completeness. Here we select high-confidence samples of radio sources (>90% reliability) to report: 38,588 radio-excess AGN in the LoTSS DR2 sample (362 HERGs, and 12,648 emission-line LERGs), together with 38,729 SFGs, and 18,726 RQAGN. We validate these results through comparison to literature using independent emission-line measurements, and to widely-adopted WISE photometric selection techniques. While our use of SDSS spectroscopy limits our current analysis to ~4 percent of the LoTSS-DR2 catalogue, our method is directly applicable to data from the forthcoming WEAVE-LOFAR survey which will obtain over a million spectra of 144 MHz selected sources.
{"title":"The LOFAR Two Metre Sky Survey Data Release 2: Probabilistic Spectral Source Classifications and Faint Radio Source Demographics","authors":"A. B. Drake, D. J. B. Smith, M. J. Hardcastle, P. N. Best, R. Kondapally, M. I. Arnaudova, S. Das, S. Shenoy, K. J. Duncan, H. J. A. Röttgering, C. Tasse","doi":"arxiv-2409.11465","DOIUrl":"https://doi.org/arxiv-2409.11465","url":null,"abstract":"We present an analysis of 152,355 radio sources identified in the second data\u0000release of the LOFAR Two Metre Sky Survey (LoTSS-DR2) with Sloan Digital Sky\u0000Survey (SDSS) spectroscopic redshifts in the range 0.00 < z < 0.57. Using Monte\u0000Carlo simulations we determine the reliability of each source exhibiting an\u0000excess in radio luminosity relative to that predicted from their Ha emission,\u0000and, for a subset of 124,023 sources we combine this measurement with a full\u0000BPT analysis. Using these two independent diagnostics we determine the\u0000reliability of each source hosting a supermassive black hole of high or low\u0000Eddington-scaled accretion rate, and combine the measurements to determine the\u0000reliability of sources belonging to each of four physical classes of objects:\u0000star forming galaxies (SFGs), radio-quiet active galactic nuclei (RQAGN), and\u0000high- or low-excitation radio galaxies (HERGs or emission-line LERGs). The\u0000result is a catalogue which enables user-defined samples of radio sources with\u0000a reliability threshold suited to their science goal e.g. prioritising purity\u0000or completeness. Here we select high-confidence samples of radio sources (>90%\u0000reliability) to report: 38,588 radio-excess AGN in the LoTSS DR2 sample (362\u0000HERGs, and 12,648 emission-line LERGs), together with 38,729 SFGs, and 18,726\u0000RQAGN. We validate these results through comparison to literature using\u0000independent emission-line measurements, and to widely-adopted WISE photometric\u0000selection techniques. While our use of SDSS spectroscopy limits our current\u0000analysis to ~4 percent of the LoTSS-DR2 catalogue, our method is directly\u0000applicable to data from the forthcoming WEAVE-LOFAR survey which will obtain\u0000over a million spectra of 144 MHz selected sources.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"62 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142269534","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}
Juno Li, Elisabete Da Cunha, Jorge González-López, Manuel Aravena, Ilse De Looze, N. M. Förster Schreiber, Rodrigo Herrera-Camus, Justin Spilker, Ken-ichi Tadaki, Loreto Barcos-Munoz, Andrew J. Battisti, Jack E. Birkin, Rebecca A. A. Bowler, Rebecca Davies, Tanio Díaz-Santos, Andrea Ferrara, Deanne B. Fisher, Jacqueline Hodge, Ryota Ikeda, Meghana Killi, Lilian Lee, Daizhong Liu, Dieter Lutz, Ikki Mitsuhashi, Thorsten Naab, Ana Posses, Monica Relaño, Manuel Solimano, Hannah Übler, Stefan Anthony van der Giessen, Vicente Villanueva
Using a combination of HST, JWST, and ALMA data, we perform spatially resolved spectral energy distributions (SED) fitting of fourteen 4
我们综合利用 HST、JWST 和 ALMA 的数据，对 ALMA（CRISTAL）大型计划[CII] Resolved ISM inStar-forming Galaxies with ALMA (CRISTAL) Large Program 的 14 个 4
{"title":"The ALMA-CRISTAL Survey: Spatially-resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies","authors":"Juno Li, Elisabete Da Cunha, Jorge González-López, Manuel Aravena, Ilse De Looze, N. M. Förster Schreiber, Rodrigo Herrera-Camus, Justin Spilker, Ken-ichi Tadaki, Loreto Barcos-Munoz, Andrew J. Battisti, Jack E. Birkin, Rebecca A. A. Bowler, Rebecca Davies, Tanio Díaz-Santos, Andrea Ferrara, Deanne B. Fisher, Jacqueline Hodge, Ryota Ikeda, Meghana Killi, Lilian Lee, Daizhong Liu, Dieter Lutz, Ikki Mitsuhashi, Thorsten Naab, Ana Posses, Monica Relaño, Manuel Solimano, Hannah Übler, Stefan Anthony van der Giessen, Vicente Villanueva","doi":"arxiv-2409.10961","DOIUrl":"https://doi.org/arxiv-2409.10961","url":null,"abstract":"Using a combination of HST, JWST, and ALMA data, we perform spatially\u0000resolved spectral energy distributions (SED) fitting of fourteen 4<z<6\u0000UV-selected main-sequence galaxies targeted by the [CII] Resolved ISM in\u0000Star-forming Galaxies with ALMA (CRISTAL) Large Program. We consistently model\u0000the emission from stars and dust in ~0.5-1kpc spatial bins to obtain maps of\u0000their physical properties. We find no offsets between the stellar masses (M*)\u0000and star formation rates (SFRs) derived from their global emission and those\u0000from adding up the values in our spatial bins, suggesting there is no bias of\u0000outshining by young stars on the derived global properties. We show that ALMA\u0000observations are important to derive robust parameter maps because they reduce\u0000the uncertainties in Ldust (hence Av and SFR). Using these maps we explore the\u0000resolved star-forming main sequence for z~5 galaxies, finding that this\u0000relation persists in typical star-forming galaxies in the early Universe. We\u0000find less obscured star formation where the M* (and SFR) surface densities are\u0000highest, typically in the central regions, contrary to the global relation\u0000between these parameters. We speculate this could be caused by feedback driving\u0000gas and dust out of these regions. However, more observations of infrared\u0000luminosities with ALMA are needed to verify this. Finally, we test empirical\u0000SFR prescriptions based on the UV+IR and [CII] line luminosity, finding they\u0000work well at the scales probed (~kpc). Our work demonstrates the usefulness of\u0000joint HST, JWST, and ALMA resolved SED modeling analyses at high redshift.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"14 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267105","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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