arXiv - PHYS - Astrophysics of Galaxies最新文献

{"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}

{"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}

{"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}

{"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}

{"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}

{"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}

{"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}

{"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}

{"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}

{"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}