arXiv - PHYS - Astrophysics of Galaxies最新文献

{"title":"Assembly of the Intracluster Light in the Horizon-AGN Simulation","authors":"Harley J. BrownUniversity of Nottingham, Garreth MartinUniversity of Nottingham, Frazer R. PearceUniversity of Nottingham, Nina A. HatchUniversity of Nottingham, Yannick M. BahéEcole Polytechnique Fédérale de Lausanne, Yohan DuboisInstitut d'Astrophysique de Paris","doi":"arxiv-2409.10607","DOIUrl":"https://doi.org/arxiv-2409.10607","url":null,"abstract":"The diffuse stellar component of galaxy clusters made up of intergalactic\u0000stars is termed the intracluster light (ICL). Though there is a developing\u0000understanding of the mechanisms by which the ICL is formed, no strong consensus\u0000has yet been reached on which objects the stars of the ICL are primarily\u0000sourced from. We investigate the assembly of the ICL starting approximately\u0000$10$ Gyr before $z=0$ in 11 galaxy clusters (halo masses between $sim1times\u000010^{14}$ M$_{odot}$ and $sim7times 10^{14}$ M$_{odot}$ at $zapprox0$) in\u0000the Horizon-AGN simulation. By tracking the stars of galaxies that fall into\u0000these clusters past cluster infall, we are able to link almost all of the\u0000$zapprox0$ ICL back to progenitor objects. Satellite stripping, mergers, and\u0000pre-processing are all found to make significant contributions to the ICL, but\u0000any contribution from in-situ star-formation directly into the ICL appears\u0000negligible. Even after compensating for resolution effects, we find that\u0000approximately $90$ per cent of the stacked ICL of the 11 clusters that is not\u0000pre-processed should come from galaxies infalling with stellar masses above\u0000$10^{9}$ M$_{odot}$, with roughly half coming from infalling galaxies with\u0000stellar masses within half a dex of $10^{11}$ M$_{odot}$. The fact that the\u0000ICL appears largely sourced from such massive objects suggests that the ICL\u0000assembly of any individual cluster may be principally stochastic.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"52 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267323","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":"First map of D$_2$H$^+$ emission revealing the true centre of a prestellar core: further insights into deuterium chemistry","authors":"L. PaganiLERMA, Arnaud BellocheMPIFR, Bérengère PariseMPIFR","doi":"arxiv-2409.10093","DOIUrl":"https://doi.org/arxiv-2409.10093","url":null,"abstract":"Context. IRAS 16293E is a rare case of a prestellar core being subjected to\u0000the effects of at least one outflow.Aims. We want to disentangle the actual\u0000structure of the core from the outflow impact and evaluate the evolutionary\u0000stage of the core. Methods. Prestellar cores being cold and depleted, the best\u0000tracers of their central regions are the two isotopologues of trihydrogren\u0000cation which are observable from the ground, ortho-H$_2$D and para-D$_2$H . We\u0000used the Atacama Pathfinder EXperiment (APEX) telescope to map the\u0000para-D$_2$H$^+$ emission in IRAS 16293E and collected James Clerk Maxwell\u0000Telescope (JCMT) archival data of ortho-H$_2$D$^+$ . We compare their emission\u0000to that of other tracers, including dust emission, and analyse their abundance\u0000with the help of a 1D radiative transfer tool. The ratio of the abundances of\u0000ortho-H$_2$D$^+$ and para-D$_2$H$^+$ can be used to estimate the stage of the\u0000chemical evolution of the core.Results. We have obtained the first complete map\u0000of para-D$_2$H$^+$ emission in a prestellar core. We compare it to a map of\u0000ortho-H$_2$D$^+$ and show their partial anti-correlation. This reveals a\u0000strongly evolved core with a para-D$_2$H$^+$/ortho-H$_2$D$^+$ abundance ratio\u0000towards the centre for which we obtain a conservative lower limit from 3.9 (at\u000012 K) up to 8.3 (at 8 K) while the high extinction of the core is indicative of\u0000a central temperature below 10 K. This ratio is higher than predicted by the\u0000known chemical models found in the literature. Para-D$_2$H$^+$ (and indirectly\u0000ortho-H$_2$D$^+$) is the only species that reveals the true centre of this\u0000core, while the emission of other molecular tracers and dust are biased by the\u0000temperature structure that results from the impact of the outflow.Conclusions.\u0000This study invites to reconsider the analysis of previous observations of this\u0000source and possibly questions the validity of the deuteration chemical models\u0000or of the reaction and inelastic collisional rate coefficients of the H$^{+3}$\u0000isotopologue family. This could impact the deuteration clock predictions for\u0000all sources.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"34 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267253","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":"A Luminous X-ray AGN in the Dwarf-Dwarf Galaxy Merger RGG 66","authors":"Seth Kimbrell, Amy Reines","doi":"arxiv-2409.10630","DOIUrl":"https://doi.org/arxiv-2409.10630","url":null,"abstract":"We present the discovery of a luminous X-ray AGN in the dwarf galaxy merger\u0000RGG 66. The black hole is predicted to have a mass of $M_{rm BH} sim 10^{5.4}\u0000M_odot$ and to be radiating close to its Eddington limit ($L_{rm bol}/L_{rm\u0000Edd} sim 0.75$). The AGN in RGG 66 is notable both for its presence in a\u0000late-stage dwarf-dwarf merger and for its luminosity of $L_{rm 2-10~keV} =\u000010^{42.2}$ erg s$^{-1}$, which is among the most powerful AGNs known in nearby\u0000dwarf galaxies. The X-ray spectrum has a best-fit photon index of $Gamma =\u00002.4$ and an intrinsic absorption of $N_H sim 10^{21}$ cm$^{-2}$. These results\u0000come from a follow-up {it Chandra X-ray Observatory} study of four\u0000irregular/disturbed dwarf galaxies with evidence for hosting AGNs based on\u0000optical spectroscopy. The remaining three dwarf galaxies do not have detectable X-ray sources with\u0000upper limits of $L_{rm 2-10~ keV} lesssim 10^{40}$ erg s$^{-1}$. Taken at\u0000face value, our results on RGG 66 suggest that mergers may trigger the most\u0000luminous of AGNs in the dwarf galaxy regime, just as they are suspected to do\u0000in more massive galaxy mergers.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"196 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267316","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":"A phenomenological model for bright galaxies in the high-redshift Universe","authors":"Georgios Panagiotis Nikopoulos, Pratika Dayal","doi":"arxiv-2409.10613","DOIUrl":"https://doi.org/arxiv-2409.10613","url":null,"abstract":"Recent observations by the James Webb Telescope (JWST) have unveiled numerous\u0000galaxy candidates between $z sim 9 - 16.5$, hinting at an over-abundance of\u0000the bright-end of the UV Luminosity Function (UV LF) $z gtrsim 11$. Possible\u0000solutions require extremely bursty star formation, these systems being\u0000dust-free, an evolving initial mass function or even cosmic variance. In this\u0000work, we develop an analytic formalism to study dust enrichment and its impact\u0000on the UV luminosity of both main-sequence early galaxies and extremely bursty\u0000star formers. Our dust model, including the key processes of dust production in\u0000type II Supernovae, dust destruction, ejection, growth and sputtering, is\u0000calibrated against the latest datasets from the Atacama Large Millimeter Array\u0000(ALMA) at $z sim 4-7$. The model has only 3 free parameters: (i) the star\u0000formation efficiency; (ii) the dust growth timescale; and (iii) the dust\u0000distribution radius. Our key results are: (i) explaining the observed UV LF\u0000requires an average star formation efficiency that increases with redshift as\u0000$f_*(z) = 10^{0.13z-3.5}$ at $z sim 5-13$ with a number of observations\u0000hinting at objects lying a factor 10 above this main-sequence. (ii) The dust\u0000enrichment of early systems is driven by dust production in SNII ejecta; growth\u0000and sputtering are the second and third most crucial processes, impacting the\u0000dust mass by 60% and 40% respectively at $z sim 7$. (iii) In our model,\u0000galaxies at $z gtrsim 9$ can still host significant amounts of dust reaching\u0000average dust-to-stellar mass ratios of 0.19% (0.14%) at $z sim 9$ ($z sim\u000011$). Dust attenuation decreases with redshift due to dust being increasingly\u0000more dispersed within the halo. (iv) the galaxies observed by ALMA at $z sim\u00007$ comprise a biased sample that is not representative of the average\u0000population that makes up the UV LF.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"49 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267318","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 Outflowing [OII] Nebulae of Compact Starburst Galaxies at z $sim$ 0.5","authors":"Serena Perrotta, Alison L. Coil, David S. N. Rupke, Wenmeng Ning, Brendan Duong, Aleksandar M. Diamond-Stanic, Drummond B. Fielding, James E. Geach, Ryan C. Hickox, John Moustakas, Gregory H. Rudnick, Paul H. Sell, Cameren N. Swiggum, Christy A. Tremonti","doi":"arxiv-2409.10013","DOIUrl":"https://doi.org/arxiv-2409.10013","url":null,"abstract":"High-velocity outflows are ubiquitous in compact, massive (M$_* sim$\u000010$^{11}$ M$_{odot}$), z $sim$ 0.5 galaxies with extreme star formation\u0000surface densities ($Sigma_{SFR} sim$ 2000 M$_{odot}$ yr$^{-1}$ kpc$^{-2}$).\u0000We have previously detected and characterized these outflows using MgII\u0000absorption lines. To probe their full extent, we present Keck/KCWI integral\u0000field spectroscopy of the [OII] and MgII emission nebulae surrounding all of\u0000the 12 galaxies in this study. We find that [OII] is more effective than MgII\u0000in tracing low surface brightness, extended emission in these galaxies. The\u0000[OII] nebulae are spatially extended beyond the stars, with radial extent\u0000R$_{90}$ between 10 and 40 kpc. The nebulae exhibit non-gravitational motions,\u0000indicating galactic outflows with maximum blueshifted velocities ranging from\u0000-335 to -1920 km s$^{-1}$. The outflow kinematics correlate with the bursty\u0000star formation histories of these galaxies. Galaxies with the most recent\u0000bursts of star formation (within the last $<$ 3 Myr) exhibit the highest\u0000central velocity dispersions ($sigma >$ 400 km s$^{-1}$), while the oldest\u0000bursts have the lowest-velocity outflows. Many galaxies exhibit both\u0000high-velocity cores and more extended, slower-moving gas indicative of multiple\u0000outflow episodes. The slower, larger outflows occurred earlier and have\u0000decelerated as they propagate into the CGM and mix on timescales $>$ 50 Myr.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"22 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142269538","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 VIRUS-dE Survey I: Stars in dwarf elliptical galaxies - 3D dynamics and radially resolved stellar initial mass functions","authors":"Mathias Lipka, Jens Thomas, Roberto Saglia, Ralf Bender, Maximilian Fabricius, Gary J. Hill, Matthias Kluge, Martin Landriau, Ximena Mazzalay, Eva Noyola, Taniya Parikh, Jan Snigula","doi":"arxiv-2409.10518","DOIUrl":"https://doi.org/arxiv-2409.10518","url":null,"abstract":"We analyse the stellar structure of a sample of dwarf ellipticals (dE)\u0000inhabiting various environments within the Virgo cluster. Integral-field\u0000observations with a high spectral resolution allow us to robustly determine\u0000their low velocity dispersions ($sim25$ km s$^{-1}$) and higher-order\u0000kinematic moments out to the half-light radius. We find the dEs exhibit a\u0000diversity in ages with the younger dEs being less enhanced than the older,\u0000suggesting a complex star formation history for those dEs that recently entered\u0000Virgo while others have been quenched shortly after reionization.\u0000Orbit-superposition modeling allowed us to recover viewing angles, stellar\u0000mass-to-light ratios (with gradients), as well as the intrinsic orbit\u0000structure. We find that the angular momentum of the dEs is strongly suppressed\u0000compared to ordinary early-type galaxies and correlates with the environment.\u0000Flattened dEs are so because of a suppressed kinetic energy perpendicular to\u0000their equatorial plane. Combining population and dynamical modeling results, we\u0000find an age-dependent stellar initial mass function (IMF) or, alternatively,\u0000evidence for a more extended star formation history for those galaxies that\u0000have had higher initial mass and/or inhabited lower density environments. dEs\u0000appear to have a spatially homogeneous stellar structure but the state they\u0000were `frozen' in as they stopped forming stars varies dramatically according to\u0000their initial conditions.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"98 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267324","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":"Deconvolving X-ray Galaxy Cluster Spectra Using a Recurrent Inference Machine","authors":"Carter Rhea, Julie Hlavacek-Larrondo, Alexandre Adam, Ralph Kraft, Akos Bogdan, Laurence Perreault-Levasseur, Marine Prunier","doi":"arxiv-2409.10711","DOIUrl":"https://doi.org/arxiv-2409.10711","url":null,"abstract":"Recent advances in machine learning algorithms have unlocked new insights in\u0000observational astronomy by allowing astronomers to probe new frontiers. In this\u0000article, we present a methodology to disentangle the intrinsic X-ray spectrum\u0000of galaxy clusters from the instrumental response function. Employing\u0000state-of-the-art modeling software and data mining techniques of the Chandra\u0000data archive, we construct a set of 100,000 mock Chandra spectra. We train a\u0000recurrent inference machine (RIM) to take in the instrumental response and mock\u0000observation and output the intrinsic X-ray spectrum. The RIM can recover the\u0000mock intrinsic spectrum below the 1-$sigma$ error threshold; moreover, the RIM\u0000reconstruction of the mock observations are indistinguishable from the\u0000observations themselves. To further test the algorithm, we deconvolve extracted\u0000spectra from the central regions of the galaxy group NGC 1550, known to have a\u0000rich X-ray spectrum, and the massive galaxy clusters Abell 1795. Despite the\u0000RIM reconstructions consistently remaining below the 1-$sigma$ noise level,\u0000the recovered intrinsic spectra did not align with modeled expectations. This\u0000discrepancy is likely attributable to the RIM's method of implicitly encoding\u0000prior information within the neural network. This approach holds promise for\u0000unlocking new possibilities in accurate spectral reconstructions and advancing\u0000our understanding of complex X-ray cosmic phenomena.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"2 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267254","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":"Candidate ram-pressure stripped galaxies in six low-redshift clusters revealed from ultraviolet imaging","authors":"Koshy George, B. M. Poggianti, A. Omizzolo, B. Vulcani, P. Côté, J. Postma, R. Smith, Y. L. Jaffe, M. Gullieuszik, A. Moretti, A. Subramaniam, P. Sreekumar, S. K. Ghosh, S. N. Tandon, J. B. Hutchings","doi":"arxiv-2409.10586","DOIUrl":"https://doi.org/arxiv-2409.10586","url":null,"abstract":"The assembly of galaxy clusters is understood to be a hierarchical process\u0000with a continuous accretion of galaxies over time, which increases the cluster\u0000size and mass. Late-type galaxies that fall into clusters can undergo\u0000ram-pressure stripping, forming extended gas tails within which star formation\u0000can happen. The number, location, and tail orientations of such galaxies\u0000provide clues about the galaxy infall process, the assembly of the cluster over\u0000time, and the consequences of infall for galaxy evolution. Here, we utilise the\u0000$sim$ 0.5 degree diameter circular field of the Ultraviolet Imaging Telescope\u0000to image six galaxy clusters at z < 0.06 that are known to contain jellyfish\u0000galaxies. We searched for stripping candidates in the ultraviolet images of\u0000these clusters, which revealed 54 candidates showing signs of unilateral\u0000extra-planar emission, due to ram-pressure stripping. Seven candidates had\u0000already been identified as likely stripping based on optical B-band imaging. We\u0000identified 47 new candidates through UV imaging. Spectroscopic redshift\u0000information is available for 39 of these candidate galaxies, of which 19 are\u0000associated with six clusters. The galaxies with spectroscopic redshifts that\u0000are not part of the clusters appear to be within structures at different\u0000redshifts identified as additional peaks in the redshift distribution of\u0000galaxies, indicating that they might be ram-pressure stripped or disturbed\u0000galaxies in other structures along the line of sight. We examine the orbital\u0000history of these galaxies based on their location in the position-velocity\u0000phase-space diagram and explore a possible connection to the orientation of the\u0000tail direction among cluster member candidates. The tails of confirmed cluster\u0000member galaxies are found to be oriented away from the cluster centre.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"3 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267320","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":"A machine learning framework to generate star cluster realisations","authors":"George P. Prodan, Mario Pasquato, Giuliano Iorio, Alessandro Ballone, Stefano Torniamenti, Ugo Niccolò Di Carlo, Michela Mapelli","doi":"arxiv-2409.10627","DOIUrl":"https://doi.org/arxiv-2409.10627","url":null,"abstract":"Context. Computational astronomy has reached the stage where running a\u0000gravitational N-body simulation of a stellar system, such as a Milky Way star\u0000cluster, is computationally feasible, but a major limiting factor that remains\u0000is the ability to set up physically realistic initial conditions. Aims. We aim\u0000to obtain realistic initial conditions for N-body simulations by taking\u0000advantage of machine learning, with emphasis on reproducing small-scale\u0000interstellar distance distributions. Methods. The computational bottleneck for\u0000obtaining such distance distributions is the hydrodynamics of star formation,\u0000which ultimately determine the features of the stars, including positions,\u0000velocities, and masses. To mitigate this issue, we introduce a new method for\u0000sampling physically realistic initial conditions from a limited set of\u0000simulations using Gaussian processes. Results. We evaluated the resulting sets\u0000of initial conditions based on whether they meet tests for physical realism. We\u0000find that direct sampling based on the learned distribution of the star\u0000features fails to reproduce binary systems. Consequently, we show that\u0000physics-informed sampling algorithms solve this issue, as they are capable of\u0000generating realisations closer to reality.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"119 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267317","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":"Finding Passive Galaxies in HI-MaNGA: The Impact of Star-Formation Rate Indicator","authors":"Nora SalemHaverford College, Karen MastersHaverford College, David StarkSTScI, Anubhav SharmaHaverford College","doi":"arxiv-2409.09574","DOIUrl":"https://doi.org/arxiv-2409.09574","url":null,"abstract":"HI-rich galaxies typically have high star-formation rates (SFR), but there\u0000exist interesting HI-rich and low star-forming (low-SF) galaxies. Previous work\u0000on a sample of these galaxies identified from HI-MaNGA (HI follow-up to the\u0000MaNGA survey) using an infrared indicator of specific-SFR (sSFR; namely\u0000W2-W3~<2) could find no single physical process to explain their unusual\u0000behaviour. The method by which galaxies are identified as low sSFR may be\u0000important in this conclusion. In this Research Note, we explore how an HI-rich,\u0000low sSFR sample of HI-MaNGA galaxies differs using H alpha, single stellar\u0000population, and ultraviolet estimators of SFR. We find that samples are\u0000statistically similar to each other so long as W2-W3~<2 is interpreted as\u0000corresponding to sSFR<10^{-11.15} yr^{-1}.","PeriodicalId":501187,"journal":{"name":"arXiv - PHYS - Astrophysics of Galaxies","volume":"33 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142267257","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}