VO FreshNew services and resources in the Virtual Observatory, as viewed from GAVO's relational registry.2024-03-28T16:40:21.053097Zivo://org.gavo.dc/registryrss/q/rssThe GAVO data center teamhttp://dc.g-vo.orggavo@ari.uni-heidelberg.dehttp://vo.uni-hd.de/registryrss/q/rss/static/logo.pngGAVO DaCHS, makerss moduleVariable Stars in Local Group Galaxies. VI.ivo://cds.vizier/j/apj/920/1522024-03-25T05:59:22ZNeeley J.R. Monelli M. Marengo M. Fiorentino G. Vivas A.K. Walker A.,Gallart C. Martinez-Vazquez C.E. Bono G. Cassisi S. Marconi M.,Dall'Ora M. Sarajedini A.<dl> <dt>Description</dt> <dd>We present the discovery of variable stars in two isolated dwarf galaxies in the outskirts of the Local Group, VV 124 and KKr 25, using observations with the Hubble Space Telescope. VV 124 hosts stellar populations with a wide range of ages (&gt;10Gyr until the present) and therefore we find all types of classical pulsators. In VV 124, we detect a total of 771 variable stars, including 78 classical Cepheids, 10 anomalous Cepheids, one Type II Cepheid, 678 RR Lyrae stars, and four eclipsing binaries. In KKr 25, we find 25 anomalous Cepheids, 46 RR Lyrae stars, and no classical Cepheids, thus the galaxy does not have a strong young population. A comparison of the variables with evolutionary tracks suggests that both galaxies may contain an intrinsic spread in metallicity, but overall are fairly metal-poor. We also present detailed simulations, which have been designed to estimate the completeness of our variable catalog. Particularly in the cases for which the observations are not deep enough to reach the main-sequence turnoff, such as the more distant Local Group dwarf galaxies, the techniques developed here can be used together with relatively shallow color-magnitude diagrams to inform on the nature of galactic populations over the full range of ages.</dd> <dt>Author(s)</dt> <dd>Neeley J.R.; Monelli M.; Marengo M.; Fiorentino G.; Vivas A.K.; Walker A.,Gallart C.; Martinez-Vazquez C.E.; Bono G.; Cassisi S.; Marconi M.,Dall'Ora M.; Sarajedini A.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apj/920/152</dd> </dl>SHELA survey. IV. Multiwavelength phot. cat.ivo://cds.vizier/j/apjs/269/462024-03-22T10:58:56ZLeung G.C.K. Finkelstein S.L. Weaver J.R. Papovich C. Larson R.L.,Chworowsky K. Ciardullo R. Gawiser E. Gronwall C. Jogee S.,Kawinwanichakij L. Somerville R.S. Wold I.G.B. Yung L.Y.A.<dl> <dt>Description</dt> <dd>We present a 0.3-4.5{mu}m 16-band photometric catalog for the Spitzer/HETDEX Exploratory Large-Area (SHELA) survey. SHELA covers an ~27deg^2^ field within the footprint of the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX). Here we present new DECam imaging and an rizKs band-selected catalog of four million sources extracted using a fully model-based approach. We validate our photometry by comparing with the model-based DECam Legacy Survey. We analyze the differences between model-based and aperture photometry by comparing with the previous SHELA catalog, finding that our model-based photometry can measure point sources to fainter fluxes and better capture the full emission of resolved sources. The catalog is 80% (50%) complete at riz ~24.7 (25.1) AB mag, and the optical photometry reaches a 5{sigma} depth of ~25.5 AB mag. We measure photometric redshifts and achieve a 1{sigma} scatter of {Delta}z/(1+z) of 0.04 with available spectroscopic redshifts at 0&lt;=z&lt;=1. This large-area, multiwavelength photometric catalog, combined with spectroscopic information from HETDEX, will enable a wide range of extragalactic science investigations.</dd> <dt>Author(s)</dt> <dd>Leung G.C.K.; Finkelstein S.L.; Weaver J.R.; Papovich C.; Larson R.L.,Chworowsky K.; Ciardullo R.; Gawiser E.; Gronwall C.; Jogee S.,Kawinwanichakij L.; Somerville R.S.; Wold I.G.B.; Yung L.Y.A.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apjs/269/46</dd> </dl>SHELA. II. DECam and IRAC multiwavelength catalogivo://cds.vizier/j/apjs/240/52024-03-22T09:21:35ZWold I.G.B. Kawinwanichakij L. Stevans M.L. Finkelstein S.L.,Papovich C. Devarakonda Y. Ciardullo R. Feldmeier J. Florez J.,Gawiser E. Gronwall C. Jogee S. Marshall J.L. Sherman S. Shipley H.V.,Somerville R.S. Valdes F. Zeimann G.R.<dl> <dt>Description</dt> <dd>We present the ugriz-band Dark Energy Camera (DECam) plus 3.6 and 4.5{mu}m IRAC catalogs for the Spitzer/HETDEX Exploratory Large-Area (SHELA) survey. SHELA covers ~24deg^2^ of the Sloan Digital Sky Survey (SDSS) "Stripe 82" region, with seven bandpasses spanning a wavelength range of 0.35 to 4.5{mu}m. SHELA falls within the footprint of the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX), which will provide spectroscopic redshifts for ~200000 Ly{alpha} emitters at 1.9&lt;z&lt;3.5 and also for ~200000 [OII] emitters at z&lt;0.5. SHELA's deep, wide-area multiwavelength images, combined with HETDEX's spectroscopic information, will facilitate many extragalactic studies, including measuring the evolution of galaxy stellar mass, halo mass, and environment from 1.5&lt;z&lt;3.5. Here we present riz-band-selected ugriz-band DECam catalogs that reach a 5{sigma} depth of ~24.5 AB mag (for point sources with an aperture that encloses 70% of the total flux) and cover 17.5deg^2^ of the overall SHELA field. We validate our DECam catalog by comparison to the DECam Legacy Survey (DECaLS) DR5 and the Dark Energy Survey (DES) DR1. We perform IRAC forced photometry with The Tractor image modeling code to measure 3.6 and 4.5{mu}m fluxes for all objects within our DECam catalog. We demonstrate the utility of our catalog by computing galaxy number counts and estimating photometric redshifts. Our photometric redshifts recover the available &lt;z&gt;=0.33 SDSS spectroscopic redshifts with a 1{sigma} scatter in {Delta}z/(1+z) of 0.04.</dd> <dt>Author(s)</dt> <dd>Wold I.G.B.; Kawinwanichakij L.; Stevans M.L.; Finkelstein S.L.,Papovich C.; Devarakonda Y.; Ciardullo R.; Feldmeier J.; Florez J.,Gawiser E.; Gronwall C.; Jogee S.; Marshall J.L.; Sherman S.; Shipley H.V.,Somerville R.S.; Valdes F.; Zeimann G.R.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apjs/240/5</dd> </dl>JADES Lyman alpha ancillary data tableivo://cds.vizier/j/a+a/683/a2382024-03-22T08:32:38ZJones G.C. Bunker A.J. Saxena A. Witstok J. Stark D.P. Arribas S.,Baker W.M. Bhatawdekar R. Bowler R. Boyett K. Cameron A.J. Carniani S.,Charlot S. Chevallard J. Curti M. Curtis-Lake E. Eisenstein D.J.,Hainline K. Hausen R. Ji Z. Johnson B.D. Kumari N. Looser T.J.,Maiolino R. Maseda M.V. Parlanti E. Rix H.-W. Robertson B.E.,Sandles L. Scholtz J. Smit R. Tacchella S. Uebler H. Williams C.C.,Willott C.<dl> <dt>Description</dt> <dd>The rest-frame UV recombination emission line Ly{alpha} can be powered by ionising photons from young massive stars in star forming galaxies, but its ability to be resonantly scattered by neutral gas complicates its interpretation. For reionization era galaxies, a neutral intergalactic medium (IGM) will scatter Lya from the line of sight, making Lya a useful probe of the neutral fraction evolution. Here, we explore Ly{alpha} in JWST/NIRSpec spectra from the ongoing JADES programme, which targets hundreds of galaxies in the well-studied GOODS-S and GOODS-N fields. These sources are UV-faint (-20.4&lt;M_UV_&lt;-16.4), and thus represent a poorly-explored class of galaxies. The low spectral resolution (R~100) spectra of a subset of 84 galaxies in GOODS-S with z_spec_&gt;5.6 (as derived with optical lines) are fit with line and continuum models, in order to search for significant line emission. Through exploration of the R100 data, we find evidence for Ly{alpha} in 17 sources. This sample allows us to place observational constraints on the fraction of galaxies with Ly{alpha} emission in the redshift range 5.6&lt;z&lt;7.5, with a decrease from z=6 to z=7. We also find a positive correlation between Ly{alpha} equivalent width and M_{UV}, as seen in other samples. These results are used to estimate the neutral gas fraction at z~7, agreeing with previous results (X_HI_~0.5-0.9).</dd> <dt>Author(s)</dt> <dd>Jones G.C.; Bunker A.J.; Saxena A.; Witstok J.; Stark D.P.; Arribas S.,Baker W.M.; Bhatawdekar R.; Bowler R.; Boyett K.; Cameron A.J.; Carniani S.,Charlot S.; Chevallard J.; Curti M.; Curtis-Lake E.; Eisenstein D.J.,Hainline K.; Hausen R.; Ji Z.; Johnson B.D.; Kumari N.; Looser T.J.,Maiolino R.; Maseda M.V.; Parlanti E.; Rix H.-W.; Robertson B.E.,Sandles L.; Scholtz J.; Smit R.; Tacchella S.; Uebler H.; Williams C.C.,Willott C.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/a+a/683/a238</dd> </dl>Cepheid Metallicity in the Leavitt Law Surveyivo://cds.vizier/j/a+a/683/a2342024-03-22T08:30:38ZBhardwaj A. Ripepi V. Testa V. Molinaro R. Marconi M. De Somma G.,Trentin E. Musella I. Storm J. Sicignano T. Catanzaro G.<dl> <dt>Description</dt> <dd>The highly debated effect of metallicity on the absolute magnitudes of classical Cepheid variables needs to be properly quantified for determining accurate and precise distances based on their Leavitt Law. Our goal is to obtain homogeneous optical and near-infrared light curves of Milky Way Cepheid variables complementing their already collected high-resolution spectroscopic metallicities as part of the C-MetaLL survey. Together with Gaia parallaxes, we investigate period-luminosity-metallicity relations for Cepheid variables at multiple wavelengths. We present homogeneous multiband (grizJHKs) time-series observations of 78 Cepheids including 49 fundamental mode variables and 29 first-overtone mode variables. These observations were collected simultaneously using the ROS2 and REMIR instruments at the Rapid Eye Mount telescope. The Cepheid sample covers a large range of distances (0.5-19.7kpc) with varying precision of parallaxes, and thus astrometry-based luminosity fits were used to derive PL and PW relations in optical Sloan (griz) and near-infrared (JHKs) filters. These empirically calibrated relations exhibit large scatter primarily due to larger uncertainties in parallaxes of distant Cepheids, but their slopes agree well with those previously determined in the literature. Using homogeneous high-resolution spectroscopic metallicities of 61 Cepheids covering -1.1&lt;[Fe/H]&lt;0.6dex, we quantified the metallicity dependence of PL and PW relations which varies between -0.30+/-0.11 (in Ks) and -0.55+/-0.12 (in z) mag/dex in grizJHKs bands. However, the metallicity dependence in the residuals of the PL and PW relations is predominantly seen for metal-poor stars ([Fe/H]&lt;-0.3dex), which also have larger parallax uncertainties. The modest sample size precludes us from separating the contribution to the residuals due to parallax uncertainties, metallicity effects, and reddening errors. While this Cepheid sample is not optimal for calibrating the Leavitt law, upcoming photometric and spectroscopic datasets of the C-MetaLL survey will allow the accurate derivation of PL and PW relations in the Sloan and near-infrared bandpasses, which will be useful for the distance measurements in the era of the Vera C. Rubin Observatory's Legacy Survey of Space and Time and upcoming extremely large telescopes.</dd> <dt>Author(s)</dt> <dd>Bhardwaj A.; Ripepi V.; Testa V.; Molinaro R.; Marconi M.; De Somma G.,Trentin E.; Musella I.; Storm J.; Sicignano T.; Catanzaro G.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/a+a/683/a234</dd> </dl>The VISTA-CFHT Stripe 82 NIR survey (VICS82)ivo://cds.vizier/j/apjs/231/72024-03-22T07:01:14ZGeach J.E. Lin Y.-T. Makler M. Kneib J.-P. Ross N.P. Wang W.-H.,Hsieh B.-C. Leauthaud A. Bundy K. McCracken H.J. Comparat J.,Caminha G.B. Hudelot P. Lin L. Van Waerbeke L. Pereira M.E.S. Mast D.<dl> <dt>Description</dt> <dd>We present the VISTA-CFHT Stripe 82 (VICS82) survey: a near-infrared (J+K_s_) survey covering 150 square degrees of the Sloan Digital Sky Survey (SDSS) equatorial Stripe 82 to an average depth of J=21.9 AB mag and K_s_=21.4 AB mag (80% completeness limits; 5{sigma} point-source depths are approximately 0.5mag brighter). VICS82 contributes to the growing legacy of multiwavelength data in the Stripe 82 footprint. The addition of near-infrared photometry to the existing SDSS Stripe 82 coadd ugriz photometry reduces the scatter in stellar mass estimates to {delta}log(M_*_)~0.3dex for galaxies with M_*_&gt;10^9^M_{sun}_ at z~0.5, and offers improvement compared to optical-only estimates out to z~1, with stellar masses constrained within a factor of approximately 2.5. When combined with other multiwavelength imaging of the Stripe, including moderate-to-deep ultraviolet (GALEX), optical and mid-infrared (Spitzer-IRAC) coverage, as well as tens of thousands of spectroscopic redshifts, VICS82 gives access to approximately 0.5Gpc^3^ of comoving volume. Some of the main science drivers of VICS82 include (a) measuring the stellar mass function of L^*^ galaxies out to z~1; (b) detecting intermediate-redshift quasars at 2&lt;~z&lt;~3.5; (c) measuring the stellar mass function and baryon census of clusters of galaxies, and (d) performing cross-correlation experiments of cosmic microwave background lensing in the optical/near-infrared that link stellar mass to large-scale dark matter structure. Here we define and describe the survey, highlight some early science results, and present the first public data release, which includes an SDSS-matched catalog as well as the calibrated pixel data themselves.</dd> <dt>Author(s)</dt> <dd>Geach J.E.; Lin Y.-T.; Makler M.; Kneib J.-P.; Ross N.P.; Wang W.-H.,Hsieh B.-C.; Leauthaud A.; Bundy K.; McCracken H.J.; Comparat J.,Caminha G.B.; Hudelot P.; Lin L.; Van Waerbeke L.; Pereira M.E.S.; Mast D.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apjs/231/7</dd> </dl>1100 days in the life of SN 2018ibbivo://cds.vizier/j/a+a/683/a2232024-03-21T09:18:00ZSchulze S. Fransson C. Kozyreva A. Chen T.-W. Yaron O. Jerkstrand A.,Gal-Yam A. Sollerman J. Yan L. Kangas T. Leloudas G. Omand C.M.B.,Smartt S.J. Yang Y. Nicholl M. Sarin N. Yao Y. Brink T.G. Sharon A.,Rossi A. Chen P. Chen Z. Cikota A. De K. Drake A.J. Filippenko A.V.,Fremling C. Freour L. Fynbo J.P.U. Ho A.Y.Q. Inserra C. Irani I.,Kuncarayakti H. Lunnan R. Mazzali P. Ofek E.O. Palazzi E. Perley D.A.,Pursiainen M. Rothberg B. Shingles L.J. Smith K. Taggart K.,Tartaglia L. Zheng W. Anderson J.P. Cassara L. Christensen E.,Djorgovski S.G. Galbany L. Gkini A. Graham M.J. Gromadzki M.,Groom S.L. Hiramatsu D. Howell D.A. Kasliwal M.M. McCully C.,Mueller-Bravo T.E. Paiano S. Paraskeva E. Pessi P.J. Polishook D.,Rau A. Rigault M. Rusholme B.<dl> <dt>Description</dt> <dd>Stars with zero-age main sequence masses between 140 and 260 solar masses are thought to explode as pair-instability supernovae (PISNe). During their thermonuclear runaway, PISNe can produce up to several tens of solar masses of radioactive nickel, resulting in luminous transients similar to some superluminous supernovae (SLSNe). Yet, no unambiguous PISN has been discovered so far. SN 2018ibb is a hydrogen-poor SLSN at z=0.166 that evolves extremely slowly compared to the hundreds of known SLSNe. Between mid 2018 and early 2022, we monitored its photometric and spectroscopic evolution from the UV to the near-infrared (NIR) with 2-10m class telescopes. SN 2018ibb radiated &gt;3*10^51^erg during its evolution, and its bolometric light curve reached &gt;2*10^44^erg/s at its peak. The long-lasting rise of &gt;93 rest-frame days implies a long diffusion time, which requires a very high total ejected mass. The PISN mechanism naturally provides both the energy source (Ni-56) and the long diffusion time. Theoretical models of PISNe make clear predictions as to their photometric and spectroscopic properties. SN 2018ibb complies with most tests on the light curves, nebular spectra and host galaxy, and potentially all tests with the interpretation we propose. Both the light curve and the spectra require 25-44 solar masses of freshly nucleosynthesised Ni-56, pointing to the explosion of a metal-poor star with a helium core mass of 120-130 solar masses at the time of death. This interpretation is also supported by the tentative detection of [CoII]-1.025um, which has never been observed in any other PISN candidate or SLSN before. We observe a significant excess in the blue part of the optical spectrum during the nebular phase, which is in tension with predictions of existing PISN models. However, we have compelling observational evidence for an eruptive mass-loss episode of the progenitor of SN 2018ibb shortly before the explosion, and our dataset reveals that the interaction of the SN ejecta with this oxygen-rich circumstellar material contributed to the observed emission. That may explain this specific discrepancy with PISN models. Powering by a central engine, such as a magnetar or a black hole, can be excluded with high confidence. This makes SN 2018ibb by far the best candidate for being a PISN, to date.</dd> <dt>Author(s)</dt> <dd>Schulze S.; Fransson C.; Kozyreva A.; Chen T.-W.; Yaron O.; Jerkstrand A.,Gal-Yam A.; Sollerman J.; Yan L.; Kangas T.; Leloudas G.; Omand C.M.B.,Smartt S.J.; Yang Y.; Nicholl M.; Sarin N.; Yao Y.; Brink T.G.; Sharon A.,Rossi A.; Chen P.; Chen Z.; Cikota A.; De K.; Drake A.J.; Filippenko A.V.,Fremling C.; Freour L.; Fynbo J.P.U.; Ho A.Y.Q.; Inserra C.; Irani I.,Kuncarayakti H.; Lunnan R.; Mazzali P.; Ofek E.O.; Palazzi E.; Perley D.A.,Pursiainen M.; Rothberg B.; Shingles L.J.; Smith K.; Taggart K.,Tartaglia L.; Zheng W.; Anderson J.P.; Cassara L.; Christensen E.,Djorgovski S.G.; Galbany L.; Gkini A.; Graham M.J.; Gromadzki M.,Groom S.L.; Hiramatsu D.; Howell D.A.; Kasliwal M.M.; McCully C.,Mueller-Bravo T.E.; Paiano S.; Paraskeva E.; Pessi P.J.; Polishook D.,Rau A.; Rigault M.; Rusholme B.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/a+a/683/a223</dd> </dl>Departure from mass-metallicity relationivo://cds.vizier/j/other/natas/8.3682024-03-20T16:40:15ZPerez-Diaz B. Perez-Montero E. Fernandez-Ontiveros J.A. Vilchez J.M.,Amorin R.<dl> <dt>Description</dt> <dd>Heavy element accumulation and stellar mass assembly are fundamental processes in the formation and evolution of galaxies. However, the key elements that govern them, such as gas accretion and outflow, are not fully understood. This is especially true for luminous and massive galaxies, which usually suffer strong feedback as massive outflows and large-scale gas accretion triggered by galaxy interactions. Using a sample of 77 luminous infrared (IR) galaxies, we derive chemical abundances using new diagnostics based on nebular IR lines, which peer through their dusty medium and allow us to include the obscured metals. In contrast to optically based studies, our analysis reveals that most luminous IR galaxies remain close to the mass-metallicity relation. Four galaxies with extreme star formation rates (&gt;60M_{sun}_/yr) in their late-merger stages show strongly depressed metallicities (12+log(O/H)~7.7-8.1) along with solar-like N/O ratios, indicative of gas mixing processes and suggesting the action of massive infall of metal-poor gas in a short phase, eventually followed by rapid enrichment. These results challenge the classical gas equilibrium scenario applied to main-sequence galaxies, suggesting that chemical enrichment and stellar-mass growth in luminous IR galaxies likely occur via mergers, driving these galaxies out of chemical equilibrium.</dd> <dt>Author(s)</dt> <dd>Perez-Diaz B.; Perez-Montero E.; Fernandez-Ontiveros J.A.; Vilchez J.M.,Amorin R.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/other/natas/8.368</dd> </dl>HST imaging and light curves of 21 SPIRITS variablesivo://cds.vizier/j/apj/928/1582024-03-20T11:51:06ZBond H.E. Jencson J.E. Whitelock P.A. Adams S.M. Bally J. Cody A.M.,Gehrz R.D. Kasliwal M.M. Masci F.J.<dl> <dt>Description</dt> <dd>The SPitzer InfraRed Intensive Transients Survey (SPIRITS) searched for luminous infrared (IR) transients and variables in nearly 200 nearby galaxies from 2014 to 2019, using the warm Spitzer telescope at 3.6 and 4.5{mu}m. Among the SPIRITS variables are IR-bright objects that are undetected in ground-based optical surveys. We classify them as (1) transients, (2) periodic variables, and (3) irregular variables. The transients include eSPecially Red Intermediate-luminosity Transient Events (SPRITEs), having maximum luminosities fainter than supernovae, red IR colors, and a wide range of outburst durations (days to years). Here we report deep optical and near-IR imaging with the Hubble Space Telescope (HST) of 21 SPIRITS variables. They were initially considered SPRITE transients, but many eventually proved instead to be periodic or irregular variables as more data were collected. HST images show most of these cool and dusty variables are associated with star-forming regions in late-type galaxies, implying an origin in massive stars. Two SPRITEs lacked optical progenitors in deep preoutburst HST images; however, one was detected during eruption at J and H, indicating a dusty object with an effective temperature of ~1050K. One faint SPRITE turned out to be a dusty classical nova. About half the HST targets proved to be periodic variables, with pulsation periods of 670-2160d; they are likely dusty asymptotic-giant-branch (AGB) stars with masses of ~5-10M_{sun}_. A few of them were warm enough to be detected in deep HST frames, but most are too cool. Out of six irregular variables, two were red supergiants with optical counterparts in HST images; four were too enshrouded for HST detection.</dd> <dt>Author(s)</dt> <dd>Bond H.E.; Jencson J.E.; Whitelock P.A.; Adams S.M.; Bally J.; Cody A.M.,Gehrz R.D.; Kasliwal M.M.; Masci F.J.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apj/928/158</dd> </dl>Optical spectroscopy of blazars for CTA. IIIivo://cds.vizier/j/a+a/683/a2222024-03-20T08:59:49ZD'Ammando F. Goldoni P. Max-Moerbeck W. Becerra Gonzalez J. Kasai E.,Williams D.A. Alvarez-Crespo N. Backes M. Barres de Almeida U.,Boisson C. Cotter G. Fallah Ramazani V. Hervet O. Lindfors E.,Mukhi-Nilo D. Pita S. Splettstoesser M. van Soelen B.<dl> <dt>Description</dt> <dd>Blazars, which include BL Lacs and flat-spectrum radio quasars (FSRQs), represent the brightest persistent extragalactic sources in the high-energy (HE; 10MeV-100GeV) and very-high-energy (VHE; E&gt;100GeV) gamma-ray sky. Due to their almost featureless optical/UV spectra, it is challenging to measure the redshifts of BL Lacs. As a result, about 50% of gamma-ray BL Lacs lack a firm measurement of this property, which is fundamental for population studies, indirect estimates of the extragalactic background light (EBL), and fundamental physics probes (e.g. searches for Lorentz-invariance violation or axion-like particles). This paper is the third in a series of papers aimed at determining the redshift of a sample of blazars selected as prime targets for future observations with the next generation, ground-based VHE gamma-ray astronomy observatory, Cherenkov Telescope Array Observatory (CTAO). The accurate determination of the redshift of these objects is an important aid in source selection and planning of future CTAO observations. Promising targets were selected following a sample selection obtained with Monte Carlo simulations of CTAO observations. The selected targets were expected to be detectable with CTAO in observations of 30 hours or less. We performed deep spectroscopic observations of 41 of these blazars using the Keck II, Lick, SALT, GTC, and ESO/VLT telescopes. We carefully searched for spectral lines in the spectra and whenever features of the host galaxy were detected, we attempted to model the properties of the host galaxy. The magnitudes of the targets at the time of the observations were also compared to their long-term light curves. Spectra from 24 objects display spectral features or a high signal-to-noise ratio (S/N). From these, 12 spectroscopic redshifts were determined, ranging from 0.2223 to 0.7018. Furthermore, 1 tentative redshift (0.6622) and 2 redshift lower limits at z&gt;0.6185 and z&gt;0.6347 were obtained. The other 9 BL Lacs showed featureless spectra, despite the high S/N (&gt;100) observations. Our comparisons with long-term optical light curves tentatively suggest that redshift measurements are more straightforward during an optical low state of the active galactic nucleus (AGN). Overall, we have determined 37 redshifts and 6 spectroscopic lower limits as part of our programme thus far.</dd> <dt>Author(s)</dt> <dd>D'Ammando F.; Goldoni P.; Max-Moerbeck W.; Becerra Gonzalez J.; Kasai E.,Williams D.A.; Alvarez-Crespo N.; Backes M.; Barres de Almeida U.,Boisson C.; Cotter G.; Fallah Ramazani V.; Hervet O.; Lindfors E.,Mukhi-Nilo D.; Pita S.; Splettstoesser M.; van Soelen B.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/a+a/683/a222</dd> </dl>MAGIC group and galaxy catalogsivo://cds.vizier/j/a+a/683/a2052024-03-20T08:58:42ZEpinat B. Contini T. Mercier W. Ciesla L. Lemaux B.C. Johnson S.D.,Richard J. Brinchmann J. Boogaard L.A. Carton D. Michel-Dansac L.,Bacon R. Krajnovic D. Finley H. Schroetter I. Ventou E.,Abril-Melgarejo V. Boselli A. Bouche N.F. Kollatschny W. Kovac K.,Paalvast M. Soucail G. Urrutia T. Weilbacher P.M.<dl> <dt>Description</dt> <dd>Galaxies migrate along cosmic web filaments from small groups to clusters, which makes the evolution of their properties look stronger as environments get denser. We introduce the MUSE gAlaxy Groups in COSMOS (MAGIC) survey built to study the impact of environment on galaxy evolution down to low stellar masses over the last eight Gyr. The MAGIC survey consists of 17 Multi-Unit Spectrocopic Exporer (MUSE) fields targeting 14 massive, known structures at intermediate redshift (0.3&lt;z&lt;0.8) in the COSMOS area, with a total on-source exposure of 67h. We securely measure redshifts for 1419 sources and identify 76 galaxy pairs and 67 groups of at least three members using a friends-of- friends algorithm. The environment of galaxies is quantified from group properties, as well as from global and local density estimators, inferred from galaxy number density and dynamics within groups. The MAGIC survey has increased the number of objects with a secure spectroscopic redshift over its footprint by a factor of ~5 compared to the previous extensive spectroscopic campaigns on the COSMOS field. Most of the new redshifts have apparent magnitudes in the z++ band z++_app&gt;21.5. The spectroscopic redshift completeness is high: in the redshift range of [OII] emitters (0.25&lt;z&lt;1.5), where most of the groups are found, it globally reaches a maximum of 80% down to z++_app_=25.9, and it locally decreases from ~100% to ~50% in magnitude bins from z++_app_=23-24 to z++_app_=25.5. We find that the fraction of quiescent galaxies increases with local density and with the time spent in groups. A morphological dichotomy is also found between bulge-dominated quiescent and disk-dominated star-forming galaxies. As environment gets denser, the peak of the stellar mass distribution shifts towards M*&gt;10^10^M_{sun}_, the fraction of galaxies with M*&lt;10^9^M_{sun}_ decreasing significantly, even for star-forming galaxies. We also highlight peculiar features such as close groups, extended nebulae, and a gravitational arc. Our results suggest that galaxies are pre- processed in groups of increasing mass before entering rich groups and clusters. We publicly release two catalogs containing the properties of galaxies and groups, respectively.</dd> <dt>Author(s)</dt> <dd>Epinat B.; Contini T.; Mercier W.; Ciesla L.; Lemaux B.C.; Johnson S.D.,Richard J.; Brinchmann J.; Boogaard L.A.; Carton D.; Michel-Dansac L.,Bacon R.; Krajnovic D.; Finley H.; Schroetter I.; Ventou E.,Abril-Melgarejo V.; Boselli A.; Bouche N.F.; Kollatschny W.; Kovac K.,Paalvast M.; Soucail G.; Urrutia T.; Weilbacher P.M.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/a+a/683/a205</dd> </dl>Spectroscopic catalog of VIPERSivo://cds.vizier/j/a+a/683/a2032024-03-20T08:54:28ZPistis F. Pollo A. Figueira M. Vergani D. Hamed M. Malek K.,Durkalec A. Donevski D. Salim S. Iovino A. Pearson W.J. Romano M.,Scodeggio M.<dl> <dt>Description</dt> <dd>We investigate the influences on the evolution of the Fundamental Metallicity Relation of different selection criteria. We used 5487 star-forming galaxies at a median redshift z~0.63 extracted from the VIMOS Public Extragalactic Redshift Survey (VIPERS) and 143774 comparison galaxies in the local Universe from the GALEX-SDSS-WISE Legacy Catalog. We employed two families of methods: parametric and non-parametric. In the parametric approaches, we compared the Fundamental Metallicity Relation projections plagued by observational biases on differently constructed control samples at various redshifts. Then, the metallicity difference between different redshifts in stellar mass-star formation rate bins. In the non-parametric approach, we related the metallicity and the normalized specific star formation rate (sSFR). To compare galaxies with the same physical properties, we normalized the median of our samples according to the median sSFR at median redshift z~0.09. Then, the galaxies with the same distance from the star-forming main sequence at their respective redshifts are compared when the sSFR is normalized according to the expected values from their respective star-forming main sequence. The methodologies implemented to construct fair, complete samples for studying the mass-metallicity relation and the Fundamental Metallicity Relation produced consistent results showing a small, but still statistically significant evolution of both relations up to z~0.63. In particular, we observed a systematic trend where the median metallicity of the sample at z=0.63 is lower than that of the local sample at the same stellar mass and star formation rate. The average difference in the metallicity of the low and intermediate redshifts is approximately 1.8 times the metallicity standard deviation of the median, of the intermediate redshift sample, in stellar mass-star formation rate bins. We confirmed this result using the Kolmogorov-Smirnov test. When we applied the stellar mass-completeness criterion to catalogs, the metallicity difference in redshifts decreased to approximately 0.96 times the metallicity standard deviation of the median, thus not statistically significant. This result may be dominated by the limited parameter space, being the lower stellar mass galaxies where the difference is larger out from the analysis. A careful reading of the results, and their underlying selection criteria, are crucial in studies of the mass-metallicity and fundamental metallicity relations. When studying the mass-metallicity and fundamental metallicity relations, we recommend using the non-parametric approach providing similar results compared to parametric prescriptions, being easier to use and results fair to interpret. The non-parametric methodology provides a convenient way to compare physical properties, with a smaller impact on observational selection biases.</dd> <dt>Author(s)</dt> <dd>Pistis F.; Pollo A.; Figueira M.; Vergani D.; Hamed M.; Malek K.,Durkalec A.; Donevski D.; Salim S.; Iovino A.; Pearson W.J.; Romano M.,Scodeggio M.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/a+a/683/a203</dd> </dl>DIBs in Gaia DR3 RVS spectraivo://cds.vizier/j/a+a/683/a1992024-03-20T08:51:51ZZhao H. Schultheis M. Qu C. Zwitter T.<dl> <dt>Description</dt> <dd>Diffuse interstellar bands (DIBs) are weak and broad interstellar absorption features in astronomical spectra that originate from unknown molecules. To measure DIBs in spectra of late-type stars more accurately and more efficiently, we developed a random forest model to isolate the DIB features from the stellar components. We applied this method to 780 thousand spectra collected by the Gaia Radial Velocity Spectrometer (RVS) that were published in the third data release (DR3). After subtracting the stellar components, we modeled the DIB at 8621{AA} ({lambda}8621) with a Gaussian function and the DIB around 8648{AA} ({lambda}8648) with a Lorentzian function. After quality control, we selected 7619 reliable measurements for DIB {lambda}8621. The equivalent width (EW) of DIB {lambda}8621 presented a moderate linear correlation with dust reddening, which was consistent with our previous measurements in Gaia DR3 and the newly focused product release. The rest-frame wavelength of DIB {lambda}8621 was updated as {lambda}0=8623.141+/-0.030{AA} in vacuum, corresponding to 8620.766{AA} in air, which was determined by 77 DIB measurements toward the Galactic anticenter. The mean uncertainty of the fit central wave-length of these 77 measurements is 0.256{AA}. With the peak-finding method and a coarse analysis, DIB {lambda}8621 was found to correlate better with the neutral hydrogen than with the molecular hydrogen (represented by ^12^CO J=(1-0) emission). We also obtained 179 reliable measurements of DIB {lambda}8648 in the RVS spectra of individual stars for the first time, further confirming this very broad DIB feature. Its EW and central wavelength presented a linear relation with those of DIB {lambda}8621. A rough estimation of {lambda}0 for DIB {lambda}8648 was 8646.31{AA} in vacuum, corresponding to 8643.93{AA} in air, assuming that the carriers of {lambda}8621 and {lambda}8648 are comoving. Finally, we confirmed the impact of stellar residuals on the DIB measurements in Gaia DR3, which led to a distortion of the DIB profile and a shift of the center (&lt;~0.5{AA}), but the EW was consistent with our new measurements. With our measurements and analyses, we propose that the approach based on machine learning can be widely applied to measure DIBs in numerous spectra from spectroscopic surveys.</dd> <dt>Author(s)</dt> <dd>Zhao H.; Schultheis M.; Qu C.; Zwitter T.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/a+a/683/a199</dd> </dl>Radial velocity follow up of HD 307842ivo://cds.vizier/j/aj/166/322024-03-20T07:44:21ZHua X. Wang S.X. Teske J.K. Gan T. Shporer A. Zhou G. Stassun K.G.,Rabus M. Howell S.B. Ziegler C. Lissauer J.J. Winn J.N. Jenkins J.M.,Ting E.B. Collins K.A. Mann A.W. Zhu W. Wang Su Butler R.P.,Crane J.D. Shectman S.A. Bouma L.G. Briceno C. Dragomir D. Fong W.,Law N. Medina J.V. Quinn S.N. Ricker G.R. Schwarz R.P. Seager S.,Sefako R. Stockdale C. Vanderspek R. Villasenor J.<dl> <dt>Description</dt> <dd>We report the confirmation of a TESS-discovered transiting super-Earth planet orbiting a mid-G star, HD307842 (TOI-784). The planet has a period of 2.8days, and the radial velocity (RV) measurements constrain the mass to be 9.67_-0.82_^+0.83^M{Earth}. We also report the discovery of an additional planet candidate on an outer orbit that is most likely nontransiting. The possible periods of the planet candidate are approximately 20^-63^days, with the corresponding RV semiamplitudes expected to range from 3.2 to 5.4m/s and minimum masses from 12.6 to 31.1 M{Earth}. The radius of the transiting planet (planet b) is 1.93_-0.09_^+0.11^R{Earth}, which results in a mean density of 7.4_-1.2_^+1.4^g/cm^3^ suggesting that TOI-784b is likely to be a rocky planet though it has a comparable radius to a sub-Neptune. We found TOI-784 b is located at the lower edge of the so-called "radius valley" in the radius versus insolation plane, which is consistent with the photoevaporation or core-powered mass-loss prediction. The TESS data did not reveal any significant transit signal of the planet candidate, and our analysis shows that the orbital inclinations of planet b and the planet candidate are 88.60deg_-0.86_^+0.84^ and &lt;~88deg^3^-89deg^2^, respectively. More RV observations are needed to determine the period and mass of the second object, and search for additional planets in this system.</dd> <dt>Author(s)</dt> <dd>Hua X.; Wang S.X.; Teske J.K.; Gan T.; Shporer A.; Zhou G.; Stassun K.G.,Rabus M.; Howell S.B.; Ziegler C.; Lissauer J.J.; Winn J.N.; Jenkins J.M.,Ting E.B.; Collins K.A.; Mann A.W.; Zhu W.; Wang Su; Butler R.P.,Crane J.D.; Shectman S.A.; Bouma L.G.; Briceno C.; Dragomir D.; Fong W.,Law N.; Medina J.V.; Quinn S.N.; Ricker G.R.; Schwarz R.P.; Seager S.,Sefako R.; Stockdale C.; Vanderspek R.; Villasenor J.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/aj/166/32</dd> </dl>g/r-band observation of AT 2019weyivo://cds.vizier/j/apj/920/1202024-03-20T07:42:04ZYao Y. Kulkarni S.R. Burdge K.B. Caiazzo I. De K. Dong D.,Fremling C. Kasliwal M.M. Kupfer T. van Roestel J. Sollerman J.,Bagdasaryan A. Bellm E.C. Cenko S.B. Drake A.J. Duev D.A.,Graham M.J. Kaye S. Masci F.J. Miranda N. Prince T.A. Riddle R.,Rusholme B. Soumagnac M.T.<dl> <dt>Description</dt> <dd>AT2019wey (SRGA J043520.9+552226, SRGE J043523.3+552234) is a transient first reported by the ATLAS optical survey in 2019 December. It rose to prominence upon detection, three months later, by the Spektrum-Roentgen-Gamma (SRG) mission in its first all-sky survey. X-ray observations reported in Yao et al. suggest that AT2019wey is a Galactic low-mass X-ray binary (LMXB) with a black hole (BH) or neutron star (NS) accretor. Here we present ultraviolet, optical, near-infrared, and radio observations of this object. We show that the companion is a short-period (P&lt;~16hr) low-mass (&lt;1M{sun}) star. We consider AT2019wey to be a candidate BH system since its locations on the Lradio-LX and Lopt-LX diagrams are closer to BH binaries than NS binaries. We demonstrate that from 2020 June to August, despite the more than 10 times brightening at radio and X-ray wavelengths, the optical luminosity of AT2019wey only increased by 1.3-1.4 times. We interpret the UV/optical emission before the brightening as thermal emission from a truncated disk in a hot accretion flow and the UV/optical emission after the brightening as reprocessing of the X-ray emission in the outer accretion disk. AT2019wey demonstrates that combining current wide-field optical surveys and SRG provides a way to discover the emerging population of short-period BH LMXB systems with faint X-ray outbursts.</dd> <dt>Author(s)</dt> <dd>Yao Y.; Kulkarni S.R.; Burdge K.B.; Caiazzo I.; De K.; Dong D.,Fremling C.; Kasliwal M.M.; Kupfer T.; van Roestel J.; Sollerman J.,Bagdasaryan A.; Bellm E.C.; Cenko S.B.; Drake A.J.; Duev D.A.,Graham M.J.; Kaye S.; Masci F.J.; Miranda N.; Prince T.A.; Riddle R.,Rusholme B.; Soumagnac M.T.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apj/920/120</dd> </dl>Light curve & radial velocities for PSRJ1810+1744ivo://cds.vizier/j/apj/908/l462024-03-20T07:38:31ZRomani R.W. Kandel D. Filippenko A.V. Brink T.G. Zheng W.<dl> <dt>Description</dt> <dd>Keck-telescope spectrophotometry of the companion of PSR-J1810+1744 shows a flat, but asymmetric light-curve maximum and a deep, narrow minimum. The maximum indicates strong gravity darkening (GD) near the L1 point, along with a heated pole and surface winds. The minimum indicates a low underlying temperature and substantial limb darkening. The GD is a consequence of extreme pulsar heating and the near-filling of the Roche lobe. Light-curve modeling gives a binary inclination i=65.7{+/-}0.4. With the Keck-measured radial-velocity amplitude Kc=462.3{+/-}2.2km/s, this gives an accurate neutron star mass MNS=2.13{+/-}0.04M{sun}, with important implications for the dense-matter equation of state. A classic direct-heating model, ignoring the L1 gravitational darkening, would predict an unphysical MNS&gt;3M{sun}. A few other "spider" pulsar binaries have similar large heating and fill factor; thus, they should be checked for such effects.</dd> <dt>Author(s)</dt> <dd>Romani R.W.; Kandel D.; Filippenko A.V.; Brink T.G.; Zheng W.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apj/908/l46</dd> </dl>X-Ray luminosities for ~41000 AGNsivo://cds.vizier/j/apj/908/1852024-03-20T07:35:38ZCarroll C.M. Hickox R.C. Masini A. Lanz L. Assef R.J. Stern D.,Chen C.-T.J. Ananna T.T.<dl> <dt>Description</dt> <dd>We present a large sample of infrared-luminous candidate active galactic nuclei (AGNs) that lack X-ray detections in Chandra, XMM-Newton, and NuSTAR fields. We selected all optically detected SDSS sources with redshift measurements, combined additional broadband photometry from WISE, UKIDSS, 2MASS, and GALEX, and modeled the spectral energy distributions (SEDs) of our sample sources. We parameterize nuclear obscuration in our SEDs with E(B-V)_AGN_ and uncover thousands of powerful obscured AGNs that lack X-ray counterparts, many of which are identified as AGN candidates based on straightforward WISE photometric criteria. Using the observed luminosity correlation between rest-frame 2-10 keV (L_X_) and rest-frame AGN 6um (L_MIR_), we estimate the intrinsic X-ray luminosities of our sample sources and combine these data with flux limits from X-ray catalogs to determine lower limits on nuclear obscuration. Using the ratio of intrinsic-to-observed X-ray luminosity (R_L_X__), we find a significant fraction of sources with column densities approaching N_H_&gt;10^24^/cm^2^, suggesting that multiwavelength observations are necessary to account for the population of heavily obscured AGNs. We simulate the underlying N_H_ distribution for the X-ray non-detected sources in our sample through survival analysis, and confirm the presence of AGN activity via X-ray stacking. Our results point to a considerable population of extremely obscured AGNs undetected by current X-ray observatories.</dd> <dt>Author(s)</dt> <dd>Carroll C.M.; Hickox R.C.; Masini A.; Lanz L.; Assef R.J.; Stern D.,Chen C.-T.J.; Ananna T.T.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apj/908/185</dd> </dl>Color-magnitude diagram for {omega} Centauriivo://cds.vizier/j/apj/908/l52024-03-20T07:31:30ZSoltis J. Casertano S. Riess A.G.<dl> <dt>Description</dt> <dd>We use data from the ESA Gaia mission Early Data Release 3 (EDR3) to measure the trigonometric parallax of {omega}Cen, the first high-precision parallax measurement for the most massive globular cluster in the Milky Way. We use a combination of positional and high-quality proper motion data from EDR3 to identify over 100000 cluster members, of which 67000 are in the magnitude and color range where EDR3 parallaxes are best calibrated. We find the estimated parallax to be robust, demonstrating good control of systematics within the color-magnitude diagram of the cluster. We find a parallax for the cluster of 0.191{+/-}0.001(statistical){+/-}0.004(systematic)mas (2.2% total uncertainty) corresponding to a distance of 5.24{+/-}0.11kpc. The parallax of {omega}Cen provides a unique opportunity to directly and geometrically calibrate the luminosity of the tip of the red giant branch (TRGB) because it is the only cluster with sufficient mass to provide enough red giant stars, more than 100 one magnitude below the tip, for a precise, model-free measurement of the tip. Combined with the preexisting and most widely used measurements of the tip and foreground Milky Way extinction, we find MI,TRGB=-3.97{+/-}0.06mag for the I-band luminosity of the blue edge. Using the TRGB luminosity calibrated from the Gaia EDR3 parallax of {omega}Cen to calibrate the luminosity of Type Ia supernovae results in a value for the Hubble constant of H0=72.1{+/-}2.0km/s/Mpc. We make the data for the stars in {omega}Cen available electronically and encourage independent analyses of the results presented here.</dd> <dt>Author(s)</dt> <dd>Soltis J.; Casertano S.; Riess A.G.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apj/908/l5</dd> </dl>Radial velocity in a Wolf-Rayet/O-star coupleivo://cds.vizier/j/apj/908/l32024-03-20T07:27:59ZRichardson N.D. Lee L. Schaefer G. Shenar T. Sander A.A.C. Hill G.M.,Fullard A.G. Monnier J.D. Anugu N. Davies C.L. Gardner T.,Lanthermann C. Kraus S. Setterholm B.R.<dl> <dt>Description</dt> <dd>We present the first visual orbit for the nitrogen-rich Wolf-Rayet binary, WR133 (WN5o+O9I), based on observations made with the CHARA Array and the MIRC-X combiner. This orbit represents the first visual orbit for a WN star and only the third Wolf-Rayet star with a visual orbit. The orbit has a period of 112.8days, a moderate eccentricity of 0.36, and a separation of a=0.79 mas on the sky. We combine the visual orbit with an SB2 orbit and Gaia parallax to find that the derived masses of the component stars are M_WR_=9.3{+/-}1.6M{odot} and M_O_=22.6{+/-}3.2M{odot}, with the large errors owing to the nearly face-on geometry of the system combined with errors in the spectroscopic parameters. We also derive an orbital parallax that is identical to the Gaia-determined distance. We present a preliminary spectral analysis and atmosphere models of the component stars, and find the mass-loss rate in agreement with polarization variability and our orbit. However, the derived masses are low compared to the spectral types and spectral model. Given the close binary nature, we suspect that WR133 should have formed through binary interactions, and represents an ideal target for testing evolutionary models given its membership in the cluster NGC6871.</dd> <dt>Author(s)</dt> <dd>Richardson N.D.; Lee L.; Schaefer G.; Shenar T.; Sander A.A.C.; Hill G.M.,Fullard A.G.; Monnier J.D.; Anugu N.; Davies C.L.; Gardner T.,Lanthermann C.; Kraus S.; Setterholm B.R.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apj/908/l3</dd> </dl>Multiply lensend quasar systems in the DESI Surveysivo://cds.vizier/j/apjs/269/612024-03-19T13:14:50ZDawes C. Storfer C. Huang X. Aldering G. Cikota A. Dey A.,Schlegel D.J.<dl> <dt>Description</dt> <dd>The time delay between multiple images of strongly lensed quasars is a powerful tool for measuring the Hubble constant (H0). To achieve H0 measurements with higher precision and accuracy using the time delay, it is crucial to expand the sample of lensed quasars. We conduct a search for strongly lensed quasars in the Dark Energy Spectroscopic Instrument (DESI) Legacy Imaging Surveys. The DESI Legacy Surveys comprise 19000deg^2^ of the extragalactic sky observed in three optical bands (g, r, and z), making it well suited for the discovery of new strongly lensed quasars. We apply an autocorrelation algorithm to ~5 million objects classified as quasars in the DESI Quasar Sample. These systems are visually inspected and ranked. Here, we present 436 new multiply lensed and binary quasar candidates, 65 of which have redshifts from Sloan Digital Sky Survey Data Release 16. We provide redshifts for an additional 18 candidates from the SuperNova Integral Field Spectrograph.</dd> <dt>Author(s)</dt> <dd>Dawes C.; Storfer C.; Huang X.; Aldering G.; Cikota A.; Dey A.,Schlegel D.J.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apjs/269/61</dd> </dl>Optical monitoring from 2020-2022 of BL Lacivo://cds.vizier/j/apjs/269/602024-03-19T13:03:35ZYuan Y.H. Du G.J. Fan J.H. Liu Y. Yang J.H. Ding G.Z. Pei Z.Y.<dl> <dt>Description</dt> <dd>BL Lacertae is a key monitoring target of the 1.26m National Astronomical Observatory-Guangzhou University Infrared/Optical telescope. Within the monitored duration from 2020 September 4 to 2022 September 28, we report 13,948 observations at the g, r, and i bands (g band: 4498, r band: 4866, i band: 4584). (1) In the monitored duration, this source is located in a very bright and variable state. The maximum variabilities are {Delta}m_g_=2.013+/-0.073mag at g band, {Delta}m_r_=1.900+/-0.049mag at r band, and {Delta}m_i_=2.279+/-0.089mag at i band. (2) Among the gri intraday lightcurves, there are 104 portions of data sets displaying intraday variabilities (IDVs), with the IDV timescales ({Delta}T) being in the range of 15.84-375.84 minutes and the biggest variable value {Delta}m=0.430+/-0.041mag. (3) The distributions of {Delta}T show frequency-dependent behavior, and with the frequency increasing, {Delta}T tend to be shorter. The variable rates (V={Delta}m}/{Delta}T) from the g band are more intense than the values (V_r_) from the r band, but are more stable than the values (V_i_) from the i band. (4) On three days (2020-September-7, 2020-September-19, and 2022-September-7), we find the intraday periodic oscillations, whose periods are around 150 minutes, 232 minutes, and 150 minutes, respectively, and which might come from the source "flickering." (5) Based on the distributions between flux densities (F_gri_) and spectral indices ({alpha}), they show the bluer-when-brighter behaviors and some uneven locations, which should come from the ministructures of the jet, the shock-induced particle acceleration, or magnetic reconnection in the jet.</dd> <dt>Author(s)</dt> <dd>Yuan Y.H.; Du G.J.; Fan J.H.; Liu Y.; Yang J.H.; Ding G.Z.; Pei Z.Y.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apjs/269/60</dd> </dl>Low-surface-brightness galaxy cand. from SDSS DR16ivo://cds.vizier/j/apjs/269/592024-03-19T12:52:02ZXing Y. Yi Z. Liang Z. Su H. Du W. He M. Liu M. Kong X. Bu Y.,Wu H.<dl> <dt>Description</dt> <dd>Low-surface-brightness galaxies (LSBGs), fainter members of the galaxy population, are thought to be numerous. However, due to their low surface brightness, the search for a wide-area sample of LSBGs is difficult, which in turn limits our ability to fully understand the formation and evolution of galaxies as well as galaxy relationships. Edge-on LSBGs, due to their unique orientation, offer an excellent opportunity to study galaxy structure and galaxy components. In this work, we utilize the You Only Look Once (YOLO) object detection algorithm to construct an edge-on LSBG detection model by training on 281 edge-on LSBGs in Sloan Digital Sky Survey (SDSS) gri-band composite images. This model achieved a recall of 94.64% and a purity of 95.38% on the test set. We searched across 938,046 gri-band images from SDSS Data Release 16 and found 52,293 candidate LSBGs. To enhance the purity of the candidate LSBGs and reduce contamination, we employed the Deep Support Vector Data Description algorithm to identify anomalies within the candidate samples. Ultimately, we compiled a catalog containing 40,759 edge-on LSBG candidates. This sample has similar characteristics to the training data set, mainly composed of blue edge-on LSBG candidates.</dd> <dt>Author(s)</dt> <dd>Xing Y.; Yi Z.; Liang Z.; Su H.; Du W.; He M.; Liu M.; Kong X.; Bu Y.,Wu H.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apjs/269/59</dd> </dl>Solar observations by Angelo Secchi. I. Sunspotivo://cds.vizier/j/apjs/269/532024-03-19T12:38:41ZErmolli I. Chatzistergos T. Giorgi F. Carrasco V.M.S. Aparicio A.J.P.,Chinnici I.<dl> <dt>Description</dt> <dd>Angelo Secchi, an Italian Jesuit and prominent scientist of the 19th century, and one of the founders of modern astrophysics, observed the Sun regularly at the Collegio Romano in Rome, Italy, for more than 25yr. Results from his observations are reported in articles published in the scientific journals of the time, as well as in drawings and personal notebooks that are stored in the historical archive of the Istituto Nazionale di Astrofisica Osservatorio Astronomico di Roma. The latter material, which reports solar observations performed from 1853-1878, includes original documents from Secchi and from a few of his close collaborators. The above unique material has recently been digitized for preservation purposes and for allowing the scientific exploitation of data not easily accessible so far. A total of more than 5400 digital images have been produced. Here we present the archival material and the new digital data derived from it. We also present results obtained from our primary analysis of the new digital data. In particular, we produced new measurements of the group number from 1853-1878, which will be available for future recalibration of the group number series.</dd> <dt>Author(s)</dt> <dd>Ermolli I.; Chatzistergos T.; Giorgi F.; Carrasco V.M.S.; Aparicio A.J.P.,Chinnici I.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apjs/269/53</dd> </dl>Ha spectroscopic obs. of Pleione from 2005-2019ivo://cds.vizier/j/apj/928/1452024-03-19T12:14:18ZMarr K.C. Jones C.E. Tycner C. Carciofi A.C. Silva A.C.F.<dl> <dt>Description</dt> <dd>We acquired H{alpha} spectroscopic observations from 2005 to 2019 showing Pleione has transitioned from a Be phase to a Be-shell phase during this period. Using the radiative transfer code hdust, we created a grid of ~100,000 disk models for Pleione. We successfully reproduced the observed transition with a disk model that varies in inclination while maintaining an equatorial density of {rho}_0_(r)=3x10^-11^(r/R_eq_)^-2.7^g/cm^3^, and an H{alpha}-emitting region extending to 15R_eq_. We use a precessing disk model to extrapolate the changing disk inclination over 120 yr and follow the variability in archival observations. The best-fit disk model precesses over a line-of-sight inclination between ~25{deg} and ~144{deg} with a precessional period of ~80.5yr. Our precessing models match some of the observed variability but fail to reproduce all of the historical data available. Therefore, we propose an ad hoc model based on our precessing disk model inspired by recent smoothed particle hydrodynamics simulations of similar systems, where the disk tears due to the tidal influence of a companion star. In this model, a single disk is slowly tilted to an angle of 30{deg} from the stellar equator over 34yr. Then, the disk is torn by the companion's tidal torque, with the outer region separating from the innermost disk. The small inner disk returns to the stellar equator as mass injection remains constant. The outer disk precesses for ~15yr before gradually dissipating. The process repeats every 34yr and reproduces all trends in Pleione's variability.</dd> <dt>Author(s)</dt> <dd>Marr K.C.; Jones C.E.; Tycner C.; Carciofi A.C.; Silva A.C.F.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apj/928/145</dd> </dl>9-month HST NUV survey of M87. I. LCs of 94 novaeivo://cds.vizier/j/apjs/269/422024-03-19T12:11:04ZShara M.M. Lessing A.M. Hounsell R. Mandel S. Zurek D. Darnley M.J.,Graur Or Hillman Y. Meyer E.T. Mikolajewska J. Neill J.D.,Prialnik D. Sparks W.<dl> <dt>Description</dt> <dd>M87 has been monitored with a cadence of 5 days over a span of 9 months through the near-ultraviolet (NUV; F275W) and optical (F606W) filters of the Wide Field Camera 3 (WFC3) of the Hubble Space Telescope. This unprecedented dataset yields the NUV and optical light and color curves of 94 M87 novae, characterizing the outburst and decline properties of the largest extragalactic nova dataset in the literature (after M31 and M81). We test and confirm nova modelers' prediction that recurrent novae cannot erupt more frequently than once every 45 days, show that there are zero rapidly recurring novae in the central ~1/3 of M87 with recurrence times &lt;130d, demonstrate that novae closely follow the K-band light of M87 to within a few arcsecs of the galaxy nucleus, show that nova NUV light curves are as heterogeneous as their optical counterparts, and usually peak 5-30d after visible light maximum, determine our observations' annual detection completeness to be 71%-77%, and measure the rate R_nova_ of nova eruptions in M87 as 352_-37_^+37^yr^-1^. The corresponding luminosity-specific classical nova rate for this galaxy is 7.91_-1.20_^+1.20^/yr/10^10^L_{sun},K_. These rates confirm that ground-based observations of extragalactic novae miss most faint, fast novae and those near the centers of galaxies. An annual M87 nova rate of 300 or more seems inescapable. A luminosity-specific nova rate of ~7-10/yr/10^10^L_{sun},K_ in all types of galaxies is indicated by the data available in 2023.</dd> <dt>Author(s)</dt> <dd>Shara M.M.; Lessing A.M.; Hounsell R.; Mandel S.; Zurek D.; Darnley M.J.,Graur Or; Hillman Y.; Meyer E.T.; Mikolajewska J.; Neill J.D.,Prialnik D.; Sparks W.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apjs/269/42</dd> </dl>NIR phot. & optical veiling in T Tauri starsivo://cds.vizier/j/apj/928/1342024-03-19T11:51:32ZSullivan K. Kraus A.L.<dl> <dt>Description</dt> <dd>Accretion is one of the defining characteristics of classical T Tauri stars, fueled by the presence of a circumstellar disk comprised of dust and gas. Accretion produces a UV and optical excess, while re-radiated emission at the inner edge of the dust component of the disk produces a near-infrared (NIR) excess. The interplay between stars and their disks helps regulate protoplanetary disk evolution and dispersal, which is key to a full understanding of planet formation. To investigate the relations between NIR excess and optical excess in both single and binary stars, we used an archival sample of spectroscopically characterized members of the Taurus star-forming region ({tau}~1-2Myr) with measured luminosities, spectral types, and optical veiling. We combined the archival sample with the Two Micron All Sky Survey and Wide-field Infrared Survey Explorer NIR photometry and high-resolution imaging surveys. We found that NIR and optical excesses are correlated in multiple NIR photometric bands, suggesting that they are closely related, likely because more massive disks have higher inner dust disk walls and are also associated with higher accretion rates. We also found that multiplicity has no impact on accretion or inner disk properties in a sample with a wide range of separations, but the sample was too small to specifically investigate close binaries, where the effects of multiplicity on disk properties should be most significant.</dd> <dt>Author(s)</dt> <dd>Sullivan K.; Kraus A.L.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apj/928/134</dd> </dl>4.7GHz OH masers in northern star formation regionsivo://cds.vizier/j/apj/928/1292024-03-19T11:38:28ZQiao H.-H. Shen Z.-Q. Breen S.L. Yang K. Chen Xi Li J.<dl> <dt>Description</dt> <dd>We have used the Shanghai Tianma Radio Telescope to search for three OH transitions at 4.7GHz toward 155 northern star formation regions. We detect 4.7GHz OH masers in 18 star formation regions, 8 of which are reported here for the first time. From these 18 sources, we detect 6 4660MHz masers, 13 4765MHz masers, and no 4750MHz masers. A further 1 source (Sgr B2N) has been re-detected with broad quasi-thermal emission in all three OH lines. W49SW was re-detected with broad quasi-thermal emission at both 4660 and 4750MHz. One source (W31, G010.626-0.387) was re-detected with quasi-thermal emission at both 4750 and 4765MHz. One source (G005.885-0.392) was first detected with quasi-thermal emission at 4660MHz. We have investigated the associations between the detected 4.7GHz OH masers with ground-state OH masers near 1.7GHz, 6.7GHz methanol masers and 22GHz water masers reported in the literature. We find that the presence of 1665MHz OH masers is a better indicator of the presence of 4.7GHz OH masers than 1720MHz OH masers. The majority of the 4.7GHz OH masers are associated with 6.7GHz methanol and/or 22GHz water masers. We have compared the characteristics of our detections with those reported previously in the literature and found that only five sources are fairly stable.</dd> <dt>Author(s)</dt> <dd>Qiao H.-H.; Shen Z.-Q.; Breen S.L.; Yang K.; Chen Xi; Li J.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apj/928/129</dd> </dl>Dynamical masses of z~0.8 galaxies from LEGA-Civo://cds.vizier/j/apj/928/1262024-03-19T11:14:41ZStraatman C.M.S. van der Wel A. van Houdt J. Bezanson R. Bell E.F.,van Dokkum P. D'Eugenio F. Franx M. Gallazzi A. de Graaff A.,Maseda M. Meidt S.E. Muzzin A. Sobral D. Wu P.-F.<dl> <dt>Description</dt> <dd>We compare dynamical mass estimates based on spatially extended stellar and ionized gas kinematics (M_dyn,*_ and M_dyn,eml_, respectively) of 157 star-forming galaxies at 0.6&lt;=z&lt;1. Compared with z~0, these galaxies have enhanced star formation rates, with stellar feedback likely affecting the dynamics of the gas. We use LEGA-C DR3, the highest-redshift data set that provides sufficiently deep measurements of a Ks-band limited sample. For M_dyn,*_, we use Jeans anisotropic multi-Gaussian expansion models. For M_dyn,eml_, we first fit a custom model of a rotating exponential disk with uniform dispersion, whose light is projected through a slit and corrected for beam smearing. We then apply an asymmetric drift correction based on assumptions common in the literature to the fitted kinematic components to obtain the circular velocity, assuming hydrostatic equilibrium. Within the half-light radius, Mdyn,eml is on average lower than M_dyn,*_, with a mean offset of -0.15+/-0.016dex and galaxy-to-galaxy scatter of 0.19dex, reflecting the combined random uncertainty. While data of higher spatial resolution are needed to understand this small offset, it supports the assumption that the galaxy-wide ionized gas kinematics do not predominantly originate from disruptive events such as star formation-driven outflows. However, a similar agreement can be obtained without modeling from the integrated emission line dispersions for axis ratios q&lt;0.8. This suggests that our current understanding of gas kinematics is not sufficient to efficiently apply asymmetric drift corrections to improve dynamical mass estimates compared with observations lacking the signal-to-noise ratio required for spatially extended dynamics.</dd> <dt>Author(s)</dt> <dd>Straatman C.M.S.; van der Wel A.; van Houdt J.; Bezanson R.; Bell E.F.,van Dokkum P.; D'Eugenio F.; Franx M.; Gallazzi A.; de Graaff A.,Maseda M.; Meidt S.E.; Muzzin A.; Sobral D.; Wu P.-F.</dd> <dt>IVOA id</dt> <dd>ivo://cds.vizier/j/apj/928/126</dd> </dl>