X. López-López, M. Bolzonella, L. Pozzetti, M. Salvato, L. Bisigello, A. Feltre, I. E. López, A. Viitanen, V. Allevato, A. Bongiorno, G. Girelli, J. Buchner, S. Charlot, F. Ricci, C. Schreiber, G. Zamorani
Aims. We present MAMBO, a flexible and efficient workflow to build empirical galaxy and Active Galactic Nuclei (AGN) mock catalogues that reproduce the physical and observational properties of these sources. Methods. We start from simulated dark matter (DM) haloes, to preserve the link with the cosmic web, and we populate them with galaxies and AGN using abundance matching techniques. We follow an empirical methodology, using stellar mass functions (SMF), host galaxy AGN mass functions and AGN accretion rate distribution functions studied at different redshifts to assign, among other properties, stellar masses, the fraction of quenched galaxies, or the AGN activity (demography, obscuration, multiwavelength emission, etc.). Results. As a proof test, we apply the method to a Millennium DM lightcone of 3.14 $rm deg^2$ up to redshift $z=10$ and down to stellar masses $mathcal{M} gtrsim 10^{7.5} , M_odot$. We show that the AGN population from the mock lightcone here presented reproduces with good accuracy various observables, such as state-of-the-art luminosity functions in the X-ray up to $z sim 7$ and in the ultraviolet up to $z sim 5$, optical/NIR colour-colour diagrams, and narrow emission line diagnostic diagrams. Finally, we demonstrate how this catalogue can be used to make useful predictions for large surveys. Using textit{Euclid} as a case example, we compute, among other forecasts, the expected surface densities of galaxies and AGN detectable in the textit{Euclid} $H_{rm E}$ band. We find that textit{Euclid} might observe (on $H_{rm E}$ only) about $10^{7}$ and $8 times 10^{7}$ Type 1 and 2 AGN respectively, and $2 times 10^{9}$ galaxies at the end of its 14 679 $rm deg^2$ Wide survey, in good agreement with other published forecasts.
目的我们介绍了 MAMBO，这是一种灵活高效的工作流程，用于建立经验星系和活动星系核（AGN）模拟星表，以再现这些星源的物理和观测特性。方法。我们从模拟暗物质（DM）光环开始，以保持与宇宙网的联系，并利用丰度匹配技术将星系和AGN填充其中。我们采用经验方法，利用在不同红移下研究的恒星质量函数（SMF）、宿主星系AGN质量函数和AGN吸积率分布函数来分配恒星质量、淬火星系比例或AGN活动（人口统计、遮挡、多波长发射等）等其他属性。结果作为证明测试，我们将该方法应用于一个红移为$z=10$、恒星质量为$mathcal{M}gtrsim 10^{7.5} 的千禧年DM光锥（Millennium DM lightcone of 3.14 $rm deg^2$）。,M_odot$。我们表明，从模拟光锥中得到的AGN种群可以很精确地再现各种观测数据，比如X射线（最高可达$z sim 7$）和紫外线（最高可达$z sim 5$）中最先进的光度函数、光学/近红外彩色图和窄发射线诊断图。最后，我们演示了如何利用这个目录为大型巡天作出有用的预测。以textit{Euclid}为例，我们计算了在textit{Euclid} $H_{rm E}$波段中可探测到的星系和AGN的预期表面密度等预测结果。我们发现，textit{Euclid}在其14 679 $rmdeg^2$ Wide巡天结束时，可能会观测到（仅在$H_{rm E}$波段上）分别为10^{7}$和8 times 10^{7}$的1类和2类AGN，以及2 times 10^{9}$的星系，这与其他已发表的预测结果非常一致。
{"title":"MAMBO -- An empirical galaxy and AGN mock catalogue for the exploitation of future surveys","authors":"X. López-López, M. Bolzonella, L. Pozzetti, M. Salvato, L. Bisigello, A. Feltre, I. E. López, A. Viitanen, V. Allevato, A. Bongiorno, G. Girelli, J. Buchner, S. Charlot, F. Ricci, C. Schreiber, G. Zamorani","doi":"arxiv-2409.06700","DOIUrl":"https://doi.org/arxiv-2409.06700","url":null,"abstract":"Aims. We present MAMBO, a flexible and efficient workflow to build empirical\u0000galaxy and Active Galactic Nuclei (AGN) mock catalogues that reproduce the\u0000physical and observational properties of these sources. Methods. We start from simulated dark matter (DM) haloes, to preserve the\u0000link with the cosmic web, and we populate them with galaxies and AGN using\u0000abundance matching techniques. We follow an empirical methodology, using\u0000stellar mass functions (SMF), host galaxy AGN mass functions and AGN accretion\u0000rate distribution functions studied at different redshifts to assign, among\u0000other properties, stellar masses, the fraction of quenched galaxies, or the AGN\u0000activity (demography, obscuration, multiwavelength emission, etc.). Results. As a proof test, we apply the method to a Millennium DM lightcone of\u00003.14 $rm deg^2$ up to redshift $z=10$ and down to stellar masses $mathcal{M}\u0000gtrsim 10^{7.5} , M_odot$. We show that the AGN population from the mock\u0000lightcone here presented reproduces with good accuracy various observables,\u0000such as state-of-the-art luminosity functions in the X-ray up to $z sim 7$ and\u0000in the ultraviolet up to $z sim 5$, optical/NIR colour-colour diagrams, and\u0000narrow emission line diagnostic diagrams. Finally, we demonstrate how this\u0000catalogue can be used to make useful predictions for large surveys. Using\u0000textit{Euclid} as a case example, we compute, among other forecasts, the\u0000expected surface densities of galaxies and AGN detectable in the\u0000textit{Euclid} $H_{rm E}$ band. We find that textit{Euclid} might observe\u0000(on $H_{rm E}$ only) about $10^{7}$ and $8 times 10^{7}$ Type 1 and 2 AGN\u0000respectively, and $2 times 10^{9}$ galaxies at the end of its 14 679 $rm\u0000deg^2$ Wide survey, in good agreement with other published forecasts.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"26 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142195381","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}
Giulia Santucci, Claudia Del P. Lagos, Katherine E. Harborne, Caro Derkenne, Adriano Poci, Sabine Thater, Richard M. McDermid, J. Trevor Mendel, Emily Wisnioski, Scott M. Croom, Anna Ferré-Mateu, Eric G. M. Muller, Jesse van de Sande, Gauri Sharma, Sarah M. Sweet, Takafumi Tsukui, Lucas M. Valenzuela, Glenn van de Ven, Tayyaba Zafar
Schwarzschild dynamical models are now regularly employed in large surveys of galaxies in the local and distant Universe to derive information on galaxies' intrinsic properties such as their orbital structure and their (dark matter and stellar) mass distribution. Comparing the internal orbital structures and mass distributions of galaxies in the distant Universe with simulations is key to understanding what physical processes are responsible for shaping galaxy properties. However it is first crucial to understand whether observationally derived properties are directly comparable with intrinsic ones in simulations. To assess this, we build Schwarzschild dynamical models for MUSE-like IFS cubes (constructed to be like those obtained by the MAGPI survey) of 75 galaxies at z ~ 0.3 from the Eagle simulations. We compare the true particle-derived properties with the galaxies' model-derived properties. In general, we find that the models can recover the true galaxy properties qualitatively well, with the exception of the enclosed dark matter, where we find a median offset of 48%, which is due to the assumed NFW profile not being able to reproduce the dark matter distribution in the inner region of the galaxies. We then compare our model-derived properties with Schwarzschild models-derived properties of observed MAGPI galaxies and find good agreement between MAGPI and Eagle: the majority of our galaxies (57%) have non-oblate shapes within 1 effective radius. More triaxial galaxies show higher fractions of hot orbits in their inner regions and tend to be more radially anisotropic.
{"title":"The MAGPI Survey: Orbital distributions, intrinsic shapes, and mass profiles for MAGPI-like Eagle galaxies using Schwarzschild dynamical models","authors":"Giulia Santucci, Claudia Del P. Lagos, Katherine E. Harborne, Caro Derkenne, Adriano Poci, Sabine Thater, Richard M. McDermid, J. Trevor Mendel, Emily Wisnioski, Scott M. Croom, Anna Ferré-Mateu, Eric G. M. Muller, Jesse van de Sande, Gauri Sharma, Sarah M. Sweet, Takafumi Tsukui, Lucas M. Valenzuela, Glenn van de Ven, Tayyaba Zafar","doi":"arxiv-2409.05940","DOIUrl":"https://doi.org/arxiv-2409.05940","url":null,"abstract":"Schwarzschild dynamical models are now regularly employed in large surveys of\u0000galaxies in the local and distant Universe to derive information on galaxies'\u0000intrinsic properties such as their orbital structure and their (dark matter and\u0000stellar) mass distribution. Comparing the internal orbital structures and mass\u0000distributions of galaxies in the distant Universe with simulations is key to\u0000understanding what physical processes are responsible for shaping galaxy\u0000properties. However it is first crucial to understand whether observationally\u0000derived properties are directly comparable with intrinsic ones in simulations.\u0000To assess this, we build Schwarzschild dynamical models for MUSE-like IFS cubes\u0000(constructed to be like those obtained by the MAGPI survey) of 75 galaxies at z\u0000~ 0.3 from the Eagle simulations. We compare the true particle-derived\u0000properties with the galaxies' model-derived properties. In general, we find\u0000that the models can recover the true galaxy properties qualitatively well, with\u0000the exception of the enclosed dark matter, where we find a median offset of\u000048%, which is due to the assumed NFW profile not being able to reproduce the\u0000dark matter distribution in the inner region of the galaxies. We then compare\u0000our model-derived properties with Schwarzschild models-derived properties of\u0000observed MAGPI galaxies and find good agreement between MAGPI and Eagle: the\u0000majority of our galaxies (57%) have non-oblate shapes within 1 effective\u0000radius. More triaxial galaxies show higher fractions of hot orbits in their\u0000inner regions and tend to be more radially anisotropic.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"87 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142195335","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}
Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham N. Diep, Nicolas Peretto, Ram K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Das R. Swagat, Jingwen Wu, Chen Wang
Filaments are believed to play a key role in high-mass star formation. We present a systematic study of the filaments and their hosting clumps in the G35 molecular complex using JCMT SCUBA-2 850 $micron$ continuum data. We identified five clouds in the complex and 91 filaments within them, some of which form 10 hub-filament systems (HFSs), each with at least 3 hub-composing filaments. We also compiled a catalogue of 350 dense clumps, 183 of which are associated with the filaments. We investigated the physical properties of the filaments and clumps, such as mass, density, and size, and their relation to star formation. We find that the global mass-length trend of the filaments is consistent with a turbulent origin, while the hub-composing filaments of high line masses ($m_{rm l},>$,230,$mathrm{M_{odot}~pc^{-1}}$) in HFSs deviate from this relation, possibly due to feedback from massive star formation. We also find that the most massive and densest clumps (R,$>$,0.2,pc, M,$>35,mathrm{M_{odot}}$, $mathrm{Sigma}>,0.05,mathrm{g~cm^{-2}}$) are located in the filaments and in the hubs of HFS with the latter bearing a higher probability of occurrence of high-mass star-forming signatures, highlighting the preferential sites of HFSs for high-mass star formation. We do not find significant variation in the clump mass surface density across different evolutionary environments of the clouds, which may reflect the balance between mass accretion and stellar feedback.
{"title":"JCMT 850 $micron$ continuum observations of density structures in the G35 molecular complex","authors":"Xianjin Shen, Hong-Li Liu, Zhiyuan Ren, Anandmayee Tej, Di Li, Hauyu Baobab Liu, Gary A. Fuller, Jinjin Xie, Sihan Jiao, Aiyuan Yang, Patrick M. Koch, Fengwei Xu, Patricio Sanhueza, Pham N. Diep, Nicolas Peretto, Ram K. Yadav, Busaba H. Kramer, Koichiro Sugiyama, Mark Rawlings, Chang Won Lee, Ken'ichi Tatematsu, Daniel Harsono, David Eden, Woojin Kwon, Chao-Wei Tsai, Glenn White, Kee-Tae Kim, Tie Liu, Ke Wang, Siju Zhang, Wenyu Jiao, Dongting Yang, Das R. Swagat, Jingwen Wu, Chen Wang","doi":"arxiv-2409.05492","DOIUrl":"https://doi.org/arxiv-2409.05492","url":null,"abstract":"Filaments are believed to play a key role in high-mass star formation. We\u0000present a systematic study of the filaments and their hosting clumps in the G35\u0000molecular complex using JCMT SCUBA-2 850 $micron$ continuum data. We\u0000identified five clouds in the complex and 91 filaments within them, some of\u0000which form 10 hub-filament systems (HFSs), each with at least 3 hub-composing\u0000filaments. We also compiled a catalogue of 350 dense clumps, 183 of which are\u0000associated with the filaments. We investigated the physical properties of the\u0000filaments and clumps, such as mass, density, and size, and their relation to\u0000star formation. We find that the global mass-length trend of the filaments is\u0000consistent with a turbulent origin, while the hub-composing filaments of high\u0000line masses ($m_{rm l},>$,230,$mathrm{M_{odot}~pc^{-1}}$) in HFSs deviate\u0000from this relation, possibly due to feedback from massive star formation. We\u0000also find that the most massive and densest clumps (R,$>$,0.2,pc,\u0000M,$>35,mathrm{M_{odot}}$, $mathrm{Sigma}>,0.05,mathrm{g~cm^{-2}}$) are\u0000located in the filaments and in the hubs of HFS with the latter bearing a\u0000higher probability of occurrence of high-mass star-forming signatures,\u0000highlighting the preferential sites of HFSs for high-mass star formation. We do\u0000not find significant variation in the clump mass surface density across\u0000different evolutionary environments of the clouds, which may reflect the\u0000balance between mass accretion and stellar feedback.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"2 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142225052","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}
Nora B. Linzer, Jeong-Gyu Kim, Chang-Goo Kim, Eve C. Ostriker
With numerical simulations that employ adaptive ray-tracing (ART) for radiative transfer at the same time as evolving gas magnetohydrodynamics, thermodynamics, and photochemistry, it is possible to obtain a high resolution view of ultraviolet (UV) fields and their effects in realistic models of the multiphase interstellar medium. Here, we analyze results from TIGRESS-NCR simulations, which follow both far-UV (FUV) wavelengths, important for photoelectric heating and PAH excitation, and the Lyman continuum (LyC), which photoionizes hydrogen. Considering two models, representing solar neighborhood and inner galaxy conditions, we characterize the spatial distribution and time variation of UV radiation fields, and quantify their correlations with gas. We compare four approximate models for the FUV to simulated values to evaluate alternatives when full ART is infeasible. By convolving FUV radiation with density, we produce mock maps of dust emission. We introduce a method to calibrate mid-IR observations, for example from JWST, to obtain high resolution gas surface density maps. We then consider the LyC radiation field, finding most of the gas exposed to this radiation to be in ionization-recombination equilibrium and to have a low neutral fraction. Additionally, we characterize the ionization parameter as a function of environment. Using a simplified model of the LyC radiation field, we produce synthetic maps of emission measure (EM). We show that the simplified model can be used to extract an estimate of the neutral fraction of the photoionized gas and mean free path of ionizing radiation from observed EM maps in galaxies.
利用自适应射线追踪（ART）进行辐射传递的数值模拟，同时演化气体磁流体力学、热力学和光化学，可以获得紫外线（UV）场及其对多相星际介质现实模型影响的高分辨率视图。在这里，我们分析了 TIGRESS-NCR 模拟的结果，这些模拟同时跟踪了对光电加热和多环芳香烃激发非常重要的远紫外（FUV）波长，以及使氢发生光离子化的莱曼连续波（LyC）波长。考虑到代表太阳附近和星系内部条件的两个模型，我们描述了紫外辐射场的空间分布和时间变化，并量化了它们与气体的相关性。我们将 FUV 的四个近似模型与模拟值进行了比较，以评估在完全 ART 不可行时的替代方案。通过卷积 FUV 辐射强度，我们绘制了尘埃辐射模拟图。我们介绍了一种校准中红外观测数据（例如来自 JWST 的观测数据）的方法，以获得高分辨率的气体表面密度图。然后，我们考虑了 LyC 辐射场，发现暴露在这种辐射下的大部分气体都处于电离-重组平衡状态，中性部分较低。此外，我们还描述了电离参数与环境的函数关系。我们利用简化的 LyC 辐射场模型，绘制了发射测量（EM）合成图。我们的研究表明，简化模型可用于从观测到的星系 EM 图中提取光离子化气体的中性部分和电离梯度平均自由路径的估计值。
{"title":"Ultraviolet Radiation Fields in Star-Forming Disk Galaxies: Numerical Simulations with TIGRESS-NCR","authors":"Nora B. Linzer, Jeong-Gyu Kim, Chang-Goo Kim, Eve C. Ostriker","doi":"arxiv-2409.05958","DOIUrl":"https://doi.org/arxiv-2409.05958","url":null,"abstract":"With numerical simulations that employ adaptive ray-tracing (ART) for\u0000radiative transfer at the same time as evolving gas magnetohydrodynamics,\u0000thermodynamics, and photochemistry, it is possible to obtain a high resolution\u0000view of ultraviolet (UV) fields and their effects in realistic models of the\u0000multiphase interstellar medium. Here, we analyze results from TIGRESS-NCR\u0000simulations, which follow both far-UV (FUV) wavelengths, important for\u0000photoelectric heating and PAH excitation, and the Lyman continuum (LyC), which\u0000photoionizes hydrogen. Considering two models, representing solar neighborhood\u0000and inner galaxy conditions, we characterize the spatial distribution and time\u0000variation of UV radiation fields, and quantify their correlations with gas. We\u0000compare four approximate models for the FUV to simulated values to evaluate\u0000alternatives when full ART is infeasible. By convolving FUV radiation with\u0000density, we produce mock maps of dust emission. We introduce a method to\u0000calibrate mid-IR observations, for example from JWST, to obtain high resolution\u0000gas surface density maps. We then consider the LyC radiation field, finding\u0000most of the gas exposed to this radiation to be in ionization-recombination\u0000equilibrium and to have a low neutral fraction. Additionally, we characterize\u0000the ionization parameter as a function of environment. Using a simplified model\u0000of the LyC radiation field, we produce synthetic maps of emission measure (EM).\u0000We show that the simplified model can be used to extract an estimate of the\u0000neutral fraction of the photoionized gas and mean free path of ionizing\u0000radiation from observed EM maps in galaxies.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142195404","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}
Qian-Hui Chen, Kathryn Grasha, Andrew J. Battisti, Emily Wisnioski, Zefeng Li, Hye-Jin Park, Brent Groves, Paul Torrey, Trevor Mendel, Barry F. Madore, Mark Seibert, Eva Sextl, Alex M. Garcia, Jeff A. Rich, Rachael L. Beaton, Lisa J. Kewley
Most star formation in the local Universe occurs in spiral galaxies, but their origin remains an unanswered question. Various theories have been proposed to explain the development of spiral arms, each predicting different spatial distributions of the interstellar medium. This study maps the star formation rate (SFR) and gas-phase metallicity of nine spiral galaxies with the TYPHOON survey to test two dominating theories: density wave theory and dynamic spiral theory. We discuss the environmental effects on our galaxies, considering reported environments and merging events. Taking advantage of the large field of view covering the entire optical disk, we quantify the fluctuation of SFR and metallicity relative to the azimuthal distance from the spiral arms. We find higher SFR and metallicity in the trailing edge of NGC~1365 (by 0.117~dex and 0.068~dex, respectively) and NGC~1566 (by 0.119~dex and 0.037~dex, respectively), which is in line with density wave theory. NGC~2442 shows a different result with higher metallicity (0.093~dex) in the leading edge, possibly attributed to an ongoing merging. The other six spiral galaxies show no statistically significant offset in SFR or metallicity, consistent with dynamic spiral theory. We also compare the behaviour of metallicity inside and outside the co-rotation radius (CR) of NGC~1365 and NGC~1566. We find comparable metallicity fluctuations near and beyond the CR of NGC~1365, indicating gravitational perturbation. NGC~1566 shows the greatest fluctuation near the CR, in line with the analytic spiral arms. Our work highlights that a combination of mechanisms explains the origin of spiral features in the local Universe.
{"title":"Quantifying azimuthal variations within the interstellar medium of z ~ 0 spiral galaxies with the TYPHOON survey","authors":"Qian-Hui Chen, Kathryn Grasha, Andrew J. Battisti, Emily Wisnioski, Zefeng Li, Hye-Jin Park, Brent Groves, Paul Torrey, Trevor Mendel, Barry F. Madore, Mark Seibert, Eva Sextl, Alex M. Garcia, Jeff A. Rich, Rachael L. Beaton, Lisa J. Kewley","doi":"arxiv-2409.05341","DOIUrl":"https://doi.org/arxiv-2409.05341","url":null,"abstract":"Most star formation in the local Universe occurs in spiral galaxies, but\u0000their origin remains an unanswered question. Various theories have been\u0000proposed to explain the development of spiral arms, each predicting different\u0000spatial distributions of the interstellar medium. This study maps the star\u0000formation rate (SFR) and gas-phase metallicity of nine spiral galaxies with the\u0000TYPHOON survey to test two dominating theories: density wave theory and dynamic\u0000spiral theory. We discuss the environmental effects on our galaxies,\u0000considering reported environments and merging events. Taking advantage of the\u0000large field of view covering the entire optical disk, we quantify the\u0000fluctuation of SFR and metallicity relative to the azimuthal distance from the\u0000spiral arms. We find higher SFR and metallicity in the trailing edge of\u0000NGC~1365 (by 0.117~dex and 0.068~dex, respectively) and NGC~1566 (by 0.119~dex\u0000and 0.037~dex, respectively), which is in line with density wave theory.\u0000NGC~2442 shows a different result with higher metallicity (0.093~dex) in the\u0000leading edge, possibly attributed to an ongoing merging. The other six spiral\u0000galaxies show no statistically significant offset in SFR or metallicity,\u0000consistent with dynamic spiral theory. We also compare the behaviour of\u0000metallicity inside and outside the co-rotation radius (CR) of NGC~1365 and\u0000NGC~1566. We find comparable metallicity fluctuations near and beyond the CR of\u0000NGC~1365, indicating gravitational perturbation. NGC~1566 shows the greatest\u0000fluctuation near the CR, in line with the analytic spiral arms. Our work\u0000highlights that a combination of mechanisms explains the origin of spiral\u0000features in the local Universe.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"23 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142195413","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}
K. R. Neralwar, D. Colombo, S. Offner, F. Wyrowski, K. M. Menten, A. Karska, M Y. Grudić, S. Neupane
Stars form in dense cores within molecular clouds and newly formed stars influence their natal environments. How stellar feedback impacts core properties and evolution is subject to extensive investigation. We performed a hierarchical clustering (dendrogram) analysis of a STARFORGE simulation modelling a giant molecular cloud to identify gas overdensities (cores) and study changes in their radius, mass, velocity dispersion, and virial parameter with respect to stellar feedback. We binned these cores on the basis of the fraction of gas affected by protostellar outflows, stellar winds, and supernovae and analysed the property distributions for each feedback bin. We find that cores that experience more feedback influence are smaller. Feedback notably enhances the velocity dispersion and virial parameter of the cores, more so than it reduces their radius. This is also evident in the linewidth-size relation, where cores in higher feedback bins exhibit higher velocities than their similarly sized pristine counterparts. We conclude that stellar feedback mechanisms, which impart momentum to the molecular cloud, simultaneously compress and disperse the dense molecular gas.
{"title":"Effects of stellar feedback on cores in STARFORGE","authors":"K. R. Neralwar, D. Colombo, S. Offner, F. Wyrowski, K. M. Menten, A. Karska, M Y. Grudić, S. Neupane","doi":"arxiv-2409.05949","DOIUrl":"https://doi.org/arxiv-2409.05949","url":null,"abstract":"Stars form in dense cores within molecular clouds and newly formed stars\u0000influence their natal environments. How stellar feedback impacts core\u0000properties and evolution is subject to extensive investigation. We performed a\u0000hierarchical clustering (dendrogram) analysis of a STARFORGE simulation\u0000modelling a giant molecular cloud to identify gas overdensities (cores) and\u0000study changes in their radius, mass, velocity dispersion, and virial parameter\u0000with respect to stellar feedback. We binned these cores on the basis of the\u0000fraction of gas affected by protostellar outflows, stellar winds, and\u0000supernovae and analysed the property distributions for each feedback bin. We\u0000find that cores that experience more feedback influence are smaller. Feedback\u0000notably enhances the velocity dispersion and virial parameter of the cores,\u0000more so than it reduces their radius. This is also evident in the\u0000linewidth-size relation, where cores in higher feedback bins exhibit higher\u0000velocities than their similarly sized pristine counterparts. We conclude that\u0000stellar feedback mechanisms, which impart momentum to the molecular cloud,\u0000simultaneously compress and disperse the dense molecular gas.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"87 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142195407","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}
Andrew W. S. Cook, Freeke van de Voort, Rüdiger Pakmor, Robert J. J. Grand
We study the dependence of the physical and observable properties of the CGM on its halo mass. We analyse 22 simulations from the Auriga suite of high resolution cosmological `zoom-in' simulations at $z=0$ with halo masses $10^{10}~text{M}_{odot}leqtext{M}_{mathrm{200c}}leq10^{12}~text{M}_{odot}$. We find a larger scatter in temperature and smaller scatter in metallicity in more massive haloes. The scatter of temperature and metallicity as a function of radius increases out to larger radii. The median and scatter of the volume-weighted density and mass-weighted radial velocity show no significant dependence on halo mass. Our results highlight that the CGM is more multiphase in haloes of higher mass. We additionally investigate column densities for HI and the metal ions CIV, OVI, MgII and SiII as a function of stellar mass and radius. We find the HI and metal ion column densities increase with stellar mass at sufficiently large radii ($Rgtrsim{0.2}$R$_{mathrm{200c}}$). We find good agreement between our HI column densities and observations outside $20$% of the virial radius and overpredict within $20$%. MgII and SiII are similarly overpredicted within $20$% of the virial radius, but drop off steeply at larger radii. Our OVI column densities underpredict observations for stellar masses between $10^{9.7}~text{M}_{odot}leqtext{M}_{star}<10^{10.8}~text{M}_{odot}$ with reasonable agreement at $10^{10.8}~text{M}_{odot}$. CIV column densities agree with observational detections above a halo mass of $10^{9.7}~text{M}_{odot}$. We find that OVI (MgII) traces the highest (lowest) temperatures, and lowest (highest) density and metallicity. OVI and CIV are photo-ionized (collisionally ionized) at low (high) halo masses with a transition to higher temperatures at $10^{11}~text{M}_{odot}$. However, there is no clear trend for the radial velocity of the ions.
{"title":"The halo mass dependence of physical and observable properties in the circumgalactic medium","authors":"Andrew W. S. Cook, Freeke van de Voort, Rüdiger Pakmor, Robert J. J. Grand","doi":"arxiv-2409.05578","DOIUrl":"https://doi.org/arxiv-2409.05578","url":null,"abstract":"We study the dependence of the physical and observable properties of the CGM\u0000on its halo mass. We analyse 22 simulations from the Auriga suite of high\u0000resolution cosmological `zoom-in' simulations at $z=0$ with halo masses\u0000$10^{10}~text{M}_{odot}leqtext{M}_{mathrm{200c}}leq10^{12}~text{M}_{odot}$.\u0000We find a larger scatter in temperature and smaller scatter in metallicity in\u0000more massive haloes. The scatter of temperature and metallicity as a function\u0000of radius increases out to larger radii. The median and scatter of the\u0000volume-weighted density and mass-weighted radial velocity show no significant\u0000dependence on halo mass. Our results highlight that the CGM is more multiphase\u0000in haloes of higher mass. We additionally investigate column densities for HI\u0000and the metal ions CIV, OVI, MgII and SiII as a function of stellar mass and\u0000radius. We find the HI and metal ion column densities increase with stellar\u0000mass at sufficiently large radii ($Rgtrsim{0.2}$R$_{mathrm{200c}}$). We find\u0000good agreement between our HI column densities and observations outside $20$%\u0000of the virial radius and overpredict within $20$%. MgII and SiII are similarly\u0000overpredicted within $20$% of the virial radius, but drop off steeply at larger\u0000radii. Our OVI column densities underpredict observations for stellar masses\u0000between\u0000$10^{9.7}~text{M}_{odot}leqtext{M}_{star}<10^{10.8}~text{M}_{odot}$ with\u0000reasonable agreement at $10^{10.8}~text{M}_{odot}$. CIV column densities\u0000agree with observational detections above a halo mass of\u0000$10^{9.7}~text{M}_{odot}$. We find that OVI (MgII) traces the highest\u0000(lowest) temperatures, and lowest (highest) density and metallicity. OVI and\u0000CIV are photo-ionized (collisionally ionized) at low (high) halo masses with a\u0000transition to higher temperatures at $10^{11}~text{M}_{odot}$. However, there\u0000is no clear trend for the radial velocity of the ions.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"31 3 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142195412","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}
Yuchen Guo, Shardha Jogee, Eden Wise, Keith Pritchett Jr., Elizabeth J. McGrath, Steven L. Finkelstein, Kartheik G. Iyer, Pablo Arrabal Haro, Micaela B. Bagley, Mark Dickinson, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, L. Y. Aaron Yung, Bren E. Backhaus, Eric F. Bell, Rachana Bhatawdekar, Yingjie Cheng, Luca Costantin, Alexander de la Vega, Mauro Giavalisco, Nimish P. Hathi, Benne W. Holwerda, Peter Kurczynski, Ray A. Lucas, Bahram Mobasher, Pablo G. Pérez-González, Fabio Pacucci
We analyze $textit{JWST}$ CEERS NIRCam images to present {the first estimate} of the observed fraction and properties of bars out to $z sim 4$. We analyze a sample of 1770 galaxies with stellar mass $M_star > 10^{10} M_odot$ at $0.5 leq z leq 4$ and identify barred galaxies via ellipse fits and visual classification of both F200W and F444W images. Our results apply mainly to bars with projected semi-major axis $a_{rm bar}$ $> 1.5 $ kpc ($sim$ 2 $times$ PSF in F200W images) that can be robustly traced by ellipse fits. For such bars, the {observed} bar fraction at $zsim$ 2-4 is low ($lesssim 10%$), and they appear to be emerging at least as early as $zsim 4$ when the Universe was $sim$ 13% of its present age. At $zsim$ 2-4, compared to our results, TNG50 simulations {predict} a significantly larger bar fraction due to a large population of small bars with $a_{rm bar}$ $< 1.5$ kpc {that we cannot robustly detect}. If such a population exists, the true bar fraction may be significantly higher than our results. At $z ge 1.5$, many barred galaxies show nearby neighbors, suggesting bars may be tidally triggered. {From $z sim 4$ to $z sim 0.5$, the observed bar fraction, average projected bar length, and projected bar strength rise.} Our results highlight the early emergence and evolution of barred galaxies and the rising importance of bar-driven secular evolution from $z sim$4 to today.
我们分析了$textit{JWST}$ CEERS NIRCam图像，首次估算了观测到的高达$z sim 4$的棒状星系的数量和性质。我们对恒星质量为 $M_star > 10^{10} 的 1770 个星系样本进行了分析。M_odot$ at $0.5 leq z leq 4$，并通过椭圆拟合以及对F200W和F444W图像的目视分类来识别棒状星系。我们的结果主要适用于投影半长轴$a_{rm bar}$ $> 1.5 $ kpc（在F200W图像中为$sim$ 2 $times$PSF）的棒状星系，它们可以通过椭圆拟合得到可靠的轨迹。对于这样的条带，在$z/sim$ 2-4时{观测到的}条带分数很低（$lesssim 10/%$），它们似乎至少早在$z/sim 4$时就出现了，当时宇宙的年龄是现在的13/%。在$z/sim$ 2-4时，与我们的结果相比，TNG50的模拟结果{预测}出了一个大得多的条带分数，这是因为有一大群a_{/rm bar}$ $< 1.5$ kpc的小条带{我们无法准确探测到}。如果存在这样一个群体，那么真实的条带分数可能会比我们的结果高得多。在$z （大于1.5$时，许多棒状星系显示出附近的邻居，这表明棒状星系可能是由潮汐触发的。{From $z sim4$ to $z sim 0.5$, the observed bar fraction, average projected bar length, and projected bar strength rise.}我们的结果突显了棒状星系的早期出现和演化，以及从$z sim$4到今天棒状星系驱动的秒演化重要性的上升。
{"title":"The Abundance and Properties of Barred Galaxies out to $z sim$ 4 Using $textit{JWST}$ CEERS Data","authors":"Yuchen Guo, Shardha Jogee, Eden Wise, Keith Pritchett Jr., Elizabeth J. McGrath, Steven L. Finkelstein, Kartheik G. Iyer, Pablo Arrabal Haro, Micaela B. Bagley, Mark Dickinson, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, L. Y. Aaron Yung, Bren E. Backhaus, Eric F. Bell, Rachana Bhatawdekar, Yingjie Cheng, Luca Costantin, Alexander de la Vega, Mauro Giavalisco, Nimish P. Hathi, Benne W. Holwerda, Peter Kurczynski, Ray A. Lucas, Bahram Mobasher, Pablo G. Pérez-González, Fabio Pacucci","doi":"arxiv-2409.06100","DOIUrl":"https://doi.org/arxiv-2409.06100","url":null,"abstract":"We analyze $textit{JWST}$ CEERS NIRCam images to present {the first\u0000estimate} of the observed fraction and properties of bars out to $z sim 4$. We\u0000analyze a sample of 1770 galaxies with stellar mass $M_star > 10^{10} M_odot$\u0000at $0.5 leq z leq 4$ and identify barred galaxies via ellipse fits and visual\u0000classification of both F200W and F444W images. Our results apply mainly to bars\u0000with projected semi-major axis $a_{rm bar}$ $> 1.5 $ kpc ($sim$ 2 $times$\u0000PSF in F200W images) that can be robustly traced by ellipse fits. For such\u0000bars, the {observed} bar fraction at $zsim$ 2-4 is low ($lesssim 10%$), and\u0000they appear to be emerging at least as early as $zsim 4$ when the Universe was\u0000$sim$ 13% of its present age. At $zsim$ 2-4, compared to our results, TNG50\u0000simulations {predict} a significantly larger bar fraction due to a large\u0000population of small bars with $a_{rm bar}$ $< 1.5$ kpc {that we cannot\u0000robustly detect}. If such a population exists, the true bar fraction may be\u0000significantly higher than our results. At $z ge 1.5$, many barred galaxies\u0000show nearby neighbors, suggesting bars may be tidally triggered. {From $z sim\u00004$ to $z sim 0.5$, the observed bar fraction, average projected bar length,\u0000and projected bar strength rise.} Our results highlight the early emergence and\u0000evolution of barred galaxies and the rising importance of bar-driven secular\u0000evolution from $z sim$4 to today.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"65 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142195405","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Anna de Graaff, Gabriel Brammer, Andrea Weibel, Zach Lewis, Michael V. Maseda, Pascal A. Oesch, Rachel Bezanson, Leindert A. Boogaard, Nikko J. Cleri, Olivia R. Cooper, Rashmi Gottumukkala, Jenny E. Greene, Michaela Hirschmann, Raphael E. Hviding, Harley Katz, Ivo Labbé, Joel Leja, Jorryt Matthee, Ian McConachie, Tim B. Miller, Rohan P. Naidu, Sedona H. Price, Hans-Walter Rix, David J. Setton, Katherine A. Suess, Bingjie Wang, Katherine E. Whitaker, Christina C. Williams
We present the Red Unknowns: Bright Infrared Extragalactic Survey (RUBIES), providing JWST/NIRSpec spectroscopy of red sources selected across ~150 arcmin$^2$ from public JWST/NIRCam imaging in the UDS and EGS fields. RUBIES novel observing strategy offers a well-quantified selection function: the survey is optimised to reach high (>70%) completeness for bright and red (F150W-F444W>2) sources that are very rare. To place these rare sources in context, we simultaneously observe a reference sample of the 23$ using only the G395M disperser. The RUBIES data reveal a highly diverse population of red sources that span a broad redshift range ($z_{spec}sim1-9$), with photometric redshift scatter and outlier fraction that are 3 times higher than for similarly bright sources that are less red. This diversity is not apparent from the photometric SEDs. Only spectroscopy reveals that the SEDs encompass a mixture of galaxies with dust-obscured star formation, extreme line emission, a lack of star formation indicating early quenching, and luminous active galactic nuclei. As a first demonstration of our broader selection function we compare the stellar masses and rest-frame U-V colours of the red sources and our reference sample: red sources are typically more massive ($M_*sim10^{10-11.5} M_odot$) across all redshifts. However, we find that the most massive systems span a wide range in U-V colour. We describe our data reduction procedure and data quality, and publicly release the reduced RUBIES data and vetted spectroscopic redshifts of the first half of the survey through the DJA.
{"title":"RUBIES: a complete census of the bright and red distant Universe with JWST/NIRSpec","authors":"Anna de Graaff, Gabriel Brammer, Andrea Weibel, Zach Lewis, Michael V. Maseda, Pascal A. Oesch, Rachel Bezanson, Leindert A. Boogaard, Nikko J. Cleri, Olivia R. Cooper, Rashmi Gottumukkala, Jenny E. Greene, Michaela Hirschmann, Raphael E. Hviding, Harley Katz, Ivo Labbé, Joel Leja, Jorryt Matthee, Ian McConachie, Tim B. Miller, Rohan P. Naidu, Sedona H. Price, Hans-Walter Rix, David J. Setton, Katherine A. Suess, Bingjie Wang, Katherine E. Whitaker, Christina C. Williams","doi":"arxiv-2409.05948","DOIUrl":"https://doi.org/arxiv-2409.05948","url":null,"abstract":"We present the Red Unknowns: Bright Infrared Extragalactic Survey (RUBIES),\u0000providing JWST/NIRSpec spectroscopy of red sources selected across ~150\u0000arcmin$^2$ from public JWST/NIRCam imaging in the UDS and EGS fields. RUBIES\u0000novel observing strategy offers a well-quantified selection function: the\u0000survey is optimised to reach high (>70%) completeness for bright and red\u0000(F150W-F444W>2) sources that are very rare. To place these rare sources in\u0000context, we simultaneously observe a reference sample of the 2<z<7 galaxy\u0000population, sampling sources at a rate that is inversely proportional to their\u0000number density in the 3D space of F444W magnitude, F150W-F444W colour, and\u0000photometric redshift. In total, RUBIES observes ~3000 targets across\u0000$1<z_{phot}<10$ with both the PRISM and G395M dispersers, and ~1500 targets at\u0000$z_{phot}>3$ using only the G395M disperser. The RUBIES data reveal a highly\u0000diverse population of red sources that span a broad redshift range\u0000($z_{spec}sim1-9$), with photometric redshift scatter and outlier fraction\u0000that are 3 times higher than for similarly bright sources that are less red.\u0000This diversity is not apparent from the photometric SEDs. Only spectroscopy\u0000reveals that the SEDs encompass a mixture of galaxies with dust-obscured star\u0000formation, extreme line emission, a lack of star formation indicating early\u0000quenching, and luminous active galactic nuclei. As a first demonstration of our\u0000broader selection function we compare the stellar masses and rest-frame U-V\u0000colours of the red sources and our reference sample: red sources are typically\u0000more massive ($M_*sim10^{10-11.5} M_odot$) across all redshifts. However, we\u0000find that the most massive systems span a wide range in U-V colour. We describe\u0000our data reduction procedure and data quality, and publicly release the reduced\u0000RUBIES data and vetted spectroscopic redshifts of the first half of the survey\u0000through the DJA.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"168 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142195409","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}
Aim: The cold molecular gas mass is one of the crucial, yet challenging parameters in galaxy evolution studies. Here, we introduce a new calibration for estimating molecular gas masses using mid-infrared (MIR) photometry. This topic is timely, as JWST now allows us to detect the MIR emission of typical main-sequence galaxies across a wide range of masses and star formation rates with modest time investments. This Letter highlights the strong synergy between ALMA and JWST for studies of dust and gas at cosmic noon. Methods: We combine a sample of 14 main sequence galaxies at z=1-3 with robust CO detections and multi-band MIR photometry, along with a literature sample at z=0-4 with CO and PAH spectroscopy, to study the relationship between PAH, CO(1-0), and total IR luminosities. PAH luminosities are derived from modeling rest-frame UV to sub-mm data. The new z=1-3 sample extends previous high-z studies to about an order-of-magnitude lower PAH and CO luminosities, into the regime of local starbursts for the first time. Results: The PAH-to-CO luminosity ratio remains constant across a wide range of luminosities, for various galaxy types, and throughout the explored redshift range. In contrast, the PAH-to-IR and CO-to-IR luminosity ratios deviate from a constant value at high L(IR). The intrinsic scatter in the L(PAH)-L'(CO) relation is 0.21 dex, with a median of 1.40, and a power-law slope of $1.07 pm 0.04$. Both the PAH-IR and CO-IR relations are sub-linear. Given the tight and uniform PAH-CO relation over ~3 orders of magnitude, we provide a recipe to estimate the cold molecular gas mass of galaxies from PAH luminosities, with a PAH-to-molecular gas conversion factor of $alpha_{rm PAH7.7} = (3.08 pm 1.08)(4.3/alpha_{rm CO}),M_{odot}/L_{odot}$. This method opens a new window to explore the gas content of galaxies beyond the local Universe using multi-wavelength JWST/MIRI imaging.
{"title":"The tight correlation of PAH and CO emission from z~0-4","authors":"Irene Shivaei, Leindert Boogaard","doi":"arxiv-2409.05710","DOIUrl":"https://doi.org/arxiv-2409.05710","url":null,"abstract":"Aim: The cold molecular gas mass is one of the crucial, yet challenging\u0000parameters in galaxy evolution studies. Here, we introduce a new calibration\u0000for estimating molecular gas masses using mid-infrared (MIR) photometry. This\u0000topic is timely, as JWST now allows us to detect the MIR emission of typical\u0000main-sequence galaxies across a wide range of masses and star formation rates\u0000with modest time investments. This Letter highlights the strong synergy between\u0000ALMA and JWST for studies of dust and gas at cosmic noon. Methods: We combine a\u0000sample of 14 main sequence galaxies at z=1-3 with robust CO detections and\u0000multi-band MIR photometry, along with a literature sample at z=0-4 with CO and\u0000PAH spectroscopy, to study the relationship between PAH, CO(1-0), and total IR\u0000luminosities. PAH luminosities are derived from modeling rest-frame UV to\u0000sub-mm data. The new z=1-3 sample extends previous high-z studies to about an\u0000order-of-magnitude lower PAH and CO luminosities, into the regime of local\u0000starbursts for the first time. Results: The PAH-to-CO luminosity ratio remains\u0000constant across a wide range of luminosities, for various galaxy types, and\u0000throughout the explored redshift range. In contrast, the PAH-to-IR and CO-to-IR\u0000luminosity ratios deviate from a constant value at high L(IR). The intrinsic\u0000scatter in the L(PAH)-L'(CO) relation is 0.21 dex, with a median of 1.40, and a\u0000power-law slope of $1.07 pm 0.04$. Both the PAH-IR and CO-IR relations are\u0000sub-linear. Given the tight and uniform PAH-CO relation over ~3 orders of\u0000magnitude, we provide a recipe to estimate the cold molecular gas mass of\u0000galaxies from PAH luminosities, with a PAH-to-molecular gas conversion factor\u0000of $alpha_{rm PAH7.7} = (3.08 pm 1.08)(4.3/alpha_{rm\u0000CO}),M_{odot}/L_{odot}$. This method opens a new window to explore the gas\u0000content of galaxies beyond the local Universe using multi-wavelength JWST/MIRI\u0000imaging.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"8 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142195197","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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