Astronomy & Astrophysics最新文献

{"title":"The GROND gamma-ray burst sample I. Overview and statistics","authors":"J. Greiner, T. Kruhler, J. Bolmer, S. Klose, P. Afonso, J. Elliott, R. Filgas, J. Graham, D. A. Kann, F. Knust","doi":"10.1051/0004-6361/202449659","DOIUrl":"https://doi.org/10.1051/0004-6361/202449659","url":null,"abstract":"A dedicated\u0000 gamma-ray burst (GRB) afterglow observing program was performed between 2007 and 2016 with GROND, a seven-channel optical and near-infrared imager at the \u0000 2.2m telescope of the Max-Planck Society at ESO/La Silla, \u0000 In this first of a series of papers, we describe the GRB observing plan,\u0000 providing first readings of all so far unpublished GRB afterglow measurements\u0000 and some observing statistics.\u0000 In total, we observed 514 GRBs with GROND, including 434 Swift -detected GRBs, representing 81 of the observable Swift sample.\u0000 For GROND-observations within 30 min of the GRB trigger, the optical/NIR\u0000 afterglow detection rate is 81 for long- and 57 for short-duration GRBs.\u0000 We report the discovery of ten new GRB\u0000 afterglows plus one candidate, along with redshift estimates (partly improved)\u0000 for four GRBs and new host detections for seven GRBs.\u0000 We identify the (already known) afterglow of GRB 140209A\u0000 as the sixth GRB exhibiting a 2175 dust feature. As a side result, we identified two blazars, with one at a redshift of z=3.8 (in the GRB 131209A field).","PeriodicalId":8585,"journal":{"name":"Astronomy & Astrophysics","volume":"28 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141796755","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":"Revisiting the dynamical masses of the transiting planets in the young AU Mic system: Potential AU,Mic b inflation at sim 20 Myr","authors":"M. Mallorquín, V. J. S. Béjar, N. Lodieu, M. Z. Zapatero Osorio, H. Yu, A. Suárez Mascareño, M. Damasso, J. Sanz-Forcada, I. Ribas, A. Reiners, A. Quirrenbach, P. Amado, J. A. Caballero, S. Aigrain, O. Barragán, S. Dreizler, Á. Fernández-Martín, E. Goffo, T. Henning, A. Kaminski, B. Klein, R. Luque, D. Montes, J. C. Morales, E. Nagel, E. Pallé, S. Reffert, M. Schlecker, A. Schweitzer","doi":"10.1051/0004-6361/202450047","DOIUrl":"https://doi.org/10.1051/0004-6361/202450047","url":null,"abstract":"Understanding planet formation is important in the context of the origin of planetary systems in general and of the Solar System in particular, as well as to predict the likelihood of finding Jupiter, Neptune, and Earth analogues around other stars. We aim to precisely determine the radii and dynamical masses of transiting planets orbiting the young M star AU,Mic using public photometric and spectroscopic datasets. We performed a joint fit analysis of the TESS and CHEOPS light curves and more than 400 high-resolution spectra collected with several telescopes and instruments. We characterise the stellar activity and physical properties (radius, mass, density) of the transiting planets in the young AU,Mic system through joint transit and radial velocity fits with Gaussian processes. We determine a radius of $R_ p b $=,4.79,pm ,0.29 R$_ a mass of p b $=,9.0,pm ,2.7 M$_ and a bulk density of $ p b $,=,0.49,pm ,0.16 $ for the innermost transiting planet AU,Mic,b. For the second known transiting planet, AU,Mic,c, we infer a radius of p c $=,2.79,pm ,0.18 R$_ a mass of p c $=,14.5,pm ,3.4 M$_ and a bulk density of $ p c $,=,3.90,pm ,1.17 $. According to theoretical models, AU,Mic,b may harbour an $ envelope larger than 5 by mass, with a fraction of rock and a fraction of water. AU,Mic,c could be made of rock and/or water and may have an $ atmosphere comprising at most 5 of its mass. AU,Mic,b has retained most of its atmosphere but might lose it over tens of millions of years due to the strong stellar radiation, while AU,Mic,c likely suffers much less photo-evaporation because it lies at a larger separation from its host. Using all the datasets in hand, we determine a 3sigma upper mass limit of p d i oplus $ for the AU,Mic 'd' TTV-candidate. In addition, we do not confirm the recently proposed existence of the planet candidate AU,Mic,'e' with an orbital period of 33.4 days. We investigated the level of the radial velocity variations and show that it is lower at longer wavelength with smaller changes from one observational campaign to another.","PeriodicalId":8585,"journal":{"name":"Astronomy & Astrophysics","volume":"27 9","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141799251","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":"Large-scale structure around the Fornax-Eridanus complex","authors":"M. A. Raj, P. Awad, R. Peletier, R. Smith, U. Kuchner, R. van de Weygaert, N.I. Libeskind, M. Canducci, P. Tino, K. Bunte","doi":"10.1051/0004-6361/202450815","DOIUrl":"https://doi.org/10.1051/0004-6361/202450815","url":null,"abstract":"Our objectives are to map the filamentary network around the Fornax-Eridanus complex and probe the influence of the local environment on galaxy morphology. We employed the novel machine-learning tool, named, 1-Dimensional, Recovery, Extraction, and Analysis of Manifolds (1-DREAM) to detect and model filaments around the Fornax cluster. We then used the morphology-density relation of galaxies to examine the variation in the galaxies' morphology with respect to their distance from the central axis of the detected filaments. We detected 27 filaments that vary in length and galaxy-number density around the Fornax-Eridanus complex. We find that 81 of galaxies in our catalogue belong to filaments and 19 of galaxies are located outside filaments. The filaments around the Fornax-Eridanus complex showcase a variety of environments: some filaments encompass groups and clusters, while others are only inhabited by galaxies in pristine filamentary environments. In this context, we reveal a well-known structure, namely: the Fornax Wall, which passes through the Dorado group, Fornax cluster, and Eridanus supergroup. With regard to the morphology of galaxies, we find that early-type galaxies (ETGs) populate high-density filaments and high-density regions of the Fornax Wall. Furthermore, the fraction of the ETG-population decreases as the distance to the central axis of the filament increases. The fraction of late-type galaxies (LTGs; 8) is lower than that of ETGs (12) at 0.5 Mpc/$h$ from the filament spine. Of the total galaxy population in filaments around the Fornax-Eridanus complex, sim 7 are ETGs and sim 24 are LTGs located in pristine environments of filaments, while sim 27 are ETGs and sim 42 are LTGs in groups and clusters within filaments. Among the galaxies in the filamentary network around the Fornax-Eridanus complex, 44 of them belong to the Fornax Wall. This study reveals the cosmic web around the Fornax cluster, which exhibits a variety of filamentary environments. With this, our research asserts that filamentary environments are heterogeneous in nature. When investigating the role of the environment on galaxy morphology, it is essential to consider both the local number-density and a galaxy's proximity to the filament spine (i.e. the filament core). Within this framework, we ascribe the observed morphological segregation in the Fornax Wall to the pre-processing of galaxies among groups embedded in it.","PeriodicalId":8585,"journal":{"name":"Astronomy & Astrophysics","volume":"39 22","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141800221","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":"Binary orbit and disks properties of the RW Aur system using ALMA observations","authors":"N. Kurtovic, S. Facchini, M. Benisty, P. Pinilla, S. Cabrit, E.L.N. Jensen, C. Dougados, R. Booth, C. N. Kimmig, C. Manara, J. E. Rodriguez","doi":"10.1051/0004-6361/202347583","DOIUrl":"https://doi.org/10.1051/0004-6361/202347583","url":null,"abstract":"The dynamical interactions between young binaries can perturb the material distribution of their circumstellar disks, and modify the planet formation process. In order to understand how planets form in multiple stellar systems, it is necessary to characterize both their binary orbit and their disks properties. In order to constrain the impact and nature of the binary interaction in the RW,Aur system (bound or unbound), we analyzed the circumstellar material at 1.3,mm wavelengths, as observed at multiple epochs by the Atacama Large (sub-)millimeter Array (ALMA). We analyzed the disk properties through parametric visibility modeling, and we used this information to constrain the dust morphology and the binary orbital period. We imaged the dust continuum emission of RW,Aur with a resolution of 3,au, and we find that the radius enclosing 90 of the flux 90 $) is 19,au and 14,au for RW,Aur,A and B, respectively. By modeling the relative distance of the disks at each epoch, we find a consistent trend of movement for the disk of RW,Aur,B moving away from the disk of RW,Aur,A at an approximate rate of $ in sky-projected distance). \u0000 By combining ALMA astrometry, historical astrometry, and the dynamical masses of each star, we constrain the RW,Aur binary stars to be most likely in a high-eccentricity elliptical orbit with a clockwise prograde orientation relative to RW,Aur,A, although low-eccentricity hyperbolic orbits are not ruled out by the astrometry. Our analysis does not exclude the possibility of a disk collision during the last interaction, which occurred $,yr ago relative to beginning of 2024. Evidence for the close interaction is found in a tentative warp of 6,deg in the inner 3,au of the disk of RW,Aur,A, in the brightness temperature of both disks, and in the morphology of the gas emission. A narrow ring that peaks at 6,au around RW,Aur,B is suggestive of captured material from the disk around RW,Aur,A.","PeriodicalId":8585,"journal":{"name":"Astronomy & Astrophysics","volume":"12 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141802093","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":"Characterising the stellar differential rotation based on largest-spot statistics from ground-based photometry","authors":"Mikko Tuomi, J. Jyri Lehtinen, W. Gregory Henry, T. Hackman","doi":"10.1051/0004-6361/202449861","DOIUrl":"https://doi.org/10.1051/0004-6361/202449861","url":null,"abstract":"Stellar spot distribution has consequences on the observable periodic signals in long-time baseline ground-based photometry. We model the statistics of the dominating spots of two young and active Solar-type stars, V889 Her and LQ Hya, in order to obtain information on the underlying spot distribution, rotation of the star, as well as the orientation of the stellar axis of spin. By calculating estimates for spot-induced periodicities in independent subsets of photometric data, we obtain statistics based on the dominating spots in each subset, giving rise to largest-spot statistics accounting for stellar geometry and rotation, including differential rotation. Our simple statistical models are able to reproduce the observed distribution of photometric signals rather well. This also enables us to estimate the dependence of angular velocity of the spots as a function of latitude. Our results indicate that V889 Her has a non-monotonic differential rotation curve with a maximum angular velocity between latitudes of 37-40 deg and lower angular velocity at the pole than the equator. Our results for LQ Hya indicate that the star rotates much like a rigid body. Furthermore, the results imply that the monotonic Solar differential rotation curve may not be a universal model for other solar-type stars. The non-monotonicity of the differential rotation of V889 Her is commonly produced in magnetohydrodynamic simulations, which indicates that our results are realistic from a theoretical perspective.","PeriodicalId":8585,"journal":{"name":"Astronomy & Astrophysics","volume":"40 26","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141800205","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":"Chandra Survey in the AKARI deep field at the North Ecliptic Pole. Optical and near-infrared identifications of X-ray sources","authors":"T. Miyaji, B. Bravo-Navarro, J. Diaz Tello, M. Krumpe, M. Herrera-Endoqui, H. Ikeda, T. Takagi, N. Oi, A. Shogaki, S. Matsuura, H. Kim, M. Malkan, H. Hwang, T. Kim, T. Ishigaki, H. Hanami, S.J. Kim, Y. Ohyama, T. Goto, H. Matsuhara","doi":"10.1051/0004-6361/202450453","DOIUrl":"https://doi.org/10.1051/0004-6361/202450453","url":null,"abstract":"We present a catalog of optical and infrared (NIR) identifications (ID) of X-ray sources in the AKARI North Ecliptic Pole (NEP) deep field detected with Chandra covering $ $ and with 0.5-2 keV flux limits ranging between $ The optical/NIR counterparts of the X-ray sources were taken from our Hyper Suprime Cam (HSC)/Subaru and Wide-Field InfraRed Camera (WIRCam)/Canada-France-Hawaii Telescope (CFHT) data because these have much more accurate source positions due to their spatial resolution than those of Chandra and longer wavelength IR data. We concentrate our identifications in the HSC $g$ band and WIRCam $K_ s $ band-based catalogs. To select the best counterpart, we utilized a novel extension of the likelihood-ratio (LR) analysis, where we used the X-ray flux as well as $g - K_ s $ colors to calculate the likelihood ratio. The spectroscopic and photometric redshifts of the counterparts are summarized in this work. In addition, simple X-ray spectroscopy was carried out on the sources with sufficient source counts. We present the resulting catalog in an electronic form. The main ID catalog contains 403 X-ray sources and includes X-ray fluxes luminosities $g$ and $K_ s $ band magnitudes, redshifts and their sources, and optical spectroscopic properties, as well as intrinsic absorption column densities and power-law indices from simple X-ray spectroscopy. The X-ray sources identified in this work include 27 Milky-Way objects, 57 type I AGNs, 131 other AGNs, and 15 galaxies. The catalog serves as a basis for further investigations of the properties of the X-ray and NIR sources in this field. We present a catalog of optical ($g$ band) and NIR ($K_ s $ band) identifications of Chandra X-ray sources in the AKARI NEP Deep field with available optical/NIR spectroscopic features and redshifts as well as the results of simple X-ray spectroscopy. In the process, we developed a novel X-ray flux-dependent likelihood-ratio analysis for selecting the most likely counterparts among candidates.","PeriodicalId":8585,"journal":{"name":"Astronomy & Astrophysics","volume":"39 18","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141800225","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":"Constraints on fast radio burst emission in the aftermath of gamma-ray bursts","authors":"B. Patricelli, M. Bernardini, M. Ferro","doi":"10.1051/0004-6361/202450444","DOIUrl":"https://doi.org/10.1051/0004-6361/202450444","url":null,"abstract":"Fast radio bursts (FRBs) are highly energetic radio transients with a duration of some milliseconds. Their physical origin is still unknown. Many models consider magnetars as possible FRB sources, which is supported by the observational association of FRBs with the galactic magnetar SGR 1935+2154. Magnetars are also thought to be the source of the power of a fraction of gamma-ray bursts (GRBs), which means that the two extreme phenomena might have a common progenitor. We placed constrains on this hypothesis by searching for possible associations between GRBs and FRBs with currently available catalogues and by estimating whether an association can be ruled out based on the lack of a coincident detection. We cross-matched all the Neil Gehrels Swift Observatory (Swift) GRBs detected so far with all the well-localised FRBs reported in the FRBSTATS catalogue, and we looked for FRB-GRB associations considering both spatial and temporal constraints. We also simulated a synthetic population of FRBs associated with Swift GRBs to estimate how likely a joint detection with current and future radio facilities is. We recovered two low-significance possible associations that were reported before from a match of the catalogues: GRB 110715A/FRB 20171209A and GRB 060502B/FRB 20190309A. However, our study shows that based on the absence of any unambiguous association so far between Swift GRBs and FRBs, we cannot exclude that the two populations are connected because of the characteristics of current GRB and FRB detectors. Currently available observational data are not sufficient to clearly exclude or confirm whether GRBs and FRBs are physically associated. In the next decade, the probability of detecting joint GRB-FRB events will be higher with new generations of GRB and FRB detectors, if any: future observations will therefore be key to placing more stringent constraints on the hypothesis that FRBs and GRBs have common progenitors.","PeriodicalId":8585,"journal":{"name":"Astronomy & Astrophysics","volume":"22 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141801658","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":"Source regions of carbonaceous meteorites and near-Earth objects","authors":"M. Broz, P. Vernazza, M. Marsset, R. Binzel, F. DeMeo, M. Birlan, F. Colas, S. Anghel, S. Bouley, C. Blanpain, J. Gattacceca, S. Jeanne, L. Jorda, J. Lecubin, A. Malgoyre, A. Steinhausser, J. Vaubaillon, B. Zanda","doi":"10.1051/0004-6361/202450532","DOIUrl":"https://doi.org/10.1051/0004-6361/202450532","url":null,"abstract":"The source regions of ordinary chondrites (sim 80 of all falls)\u0000and large S-type near-Earth objects (NEOs; sim 30)\u0000have recently been identified\u0000with three young asteroid families (Karin, Koronis, Massalia)\u0000being at the origin of most ordinary chondrite falls. The present work is a continuation of our previous studies\u0000and aims to determine the source regions of the remaining meteorite and NEO classes,\u0000with an emphasis on carbonaceous chondrites\u0000(CM, CI, CO, CV, CK, CR, CH, CB, or C-ungrouped). We studied 38 individual asteroid families, including young and old ones,\u0000and determined their contributions to the NEO populations at metre and kilometre sizes\u0000using collisional and orbital models.\u0000Our models are in agreement with\u0000spectroscopic observations of NEOs,\u0000cosmic-ray exposure ages of meteorites,\u0000statistics of bolides,\u0000infrared emission from dust bands,\u0000composition of interplanetary dust particles (IDPs), and\u0000abundance of extraterrestrial helium-3. We identified the Veritas, Polana, and Eos families\u0000as the primary sources of CM/CR, CI, and CO/CV/CK chondrites, respectively.\u0000Substantial contributions are also expected from\u0000CM-like K\"onig and CI-like Clarissa, Misa, and Hoffmeister families. The source regions of kilometre-sized bodies are generally different. The Adeona family is by far the main source of CM-like NEOs, whereas the Polana (low-i) and Euphrosyne (high-i) families are at the origin of most CI-like NEOs. The Polana family is the likely source of both Ryugu and Bennu. We were able to link spectroscopically and dynamically several NEOs to the Baptistina family. Finally, it appears that the pre-atmospheric flux of carbonaceous chondrites at metre sizes is about the same as that of ordinary chondrites. Given the difference in fall statistics between the two groups (80 versus 4.4), this implies either substantial atmospheric fragmentation of carbonaceous bodies at the level of sim MPa $\u0000or destruction by thermal cracking and water desorption. The source regions of most meteorites and kilometre-sized NEOs have now been determined,\u0000including some minor classes such as\u0000enstatite chondrites and achondrites (Nysa, Hungaria),\u0000acapulcoites and lodranites (Iannini).\u0000Future work should focus on the few remaining classes (essentially, iron meteorites, pallasites, and ureilites).","PeriodicalId":8585,"journal":{"name":"Astronomy & Astrophysics","volume":"36 50","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141800373","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^3COSMOS: Dust mass function and dust mass density at 0.5","authors":"A. Traina, B. Magnelli, C. Gruppioni, I. Delvecchio, M. Parente, F. Calura, L. Bisigello, A. Feltre, F. Pozzi, L. Vallini","doi":"10.1051/0004-6361/202451113","DOIUrl":"https://doi.org/10.1051/0004-6361/202451113","url":null,"abstract":"Although dust in galaxies represents only a few percent of the total baryonic mass, it plays a crucial role in the physical processes occurring in galaxies. Studying the dust content of galaxies, particularly at high $z$, is therefore crucial for understanding the link between dust production, obscured star formation, and the build-up of galaxy stellar mass. We study the dust properties (mass and temperature) of the largest Atacama Large Millimeter/submillimeter Array (ALMA)-selected sample of star-forming galaxies available from the archive (A$^3$COSMOS), and we derive the dust mass function and dust mass density of galaxies from $z=0.5,-,6$. We fit the spectral energy distribution (SED) with the CIGALE code to constrain the dust mass and temperature of the A$^3$COSMOS galaxy sample based on the UV-to-near-infrared photometric coverage of each galaxy combined with the ALMA (and Herschel when available) coverage of the Rayleigh-Jeans tail of their dust-continuum emission. We then computed and fit the dust mass function by combining the A$^3$COSMOS and the most recent Herschel samples in order to obtain the best estimate of the integrated dust mass density up to $z The dust masses in galaxies in lie between $ 10^8$ and $ $ M$_ odot $. From the SED fitting, we were also able to derive a dust temperature. The distribution of the dust temperature peaks at $ 30-35$K. The dust mass function at $z=0.5,-,6$ evolves with an increase in $M^*$ and a decrease in the number density ($ ^*$), and it agrees well with literature estimates. The dust mass density decreases smoothly in its evolution from $z 0.5$ to $z 6$, which is steeper than what is found by models at $z","PeriodicalId":8585,"journal":{"name":"Astronomy & Astrophysics","volume":"50 9","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141798952","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":"Resolving double-peaked emission line galaxies using MaNGA. I. Mechanisms of star formation quenching","authors":"Barbara Mazzilli Ciraulo, A. Melchior, F. Combes, Daniel Maschmann","doi":"10.1051/0004-6361/202142892","DOIUrl":"https://doi.org/10.1051/0004-6361/202142892","url":null,"abstract":"Understanding the relationship between quenching mechanisms that transform star-forming galaxies into quiescent ones and galaxy properties remains a challenge. \u0000\u0000We investigate the gas and stellar properties of 69 double-peaked galaxies selected from the Sloan Digital Sky Survey (SDSS) and observed as part of the Mapping Nearby Galaxies at APO (MaNGA) survey to elucidate the mechanisms driving star formation quenching within these systems. We study their star formation activity along with their physical properties: colour, morphology, environment, stellar age, and gas ionisation diagnostics. \u0000We find that these 69 double-peaked MaNGA galaxies encompass a higher fraction of galaxies in the green valley, based on the corrected NUV-$r$ colour, compared to our defined control samples of single-peaked emission line galaxies. This green colour traces intermediate stellar populations compared to blue and red galaxies, as indicated by the D$_n(4000)$ index. These green galaxies show no recent star formation bursts within the last 2 Gyr. They exhibit emission line ratios that are suggestive of both ongoing star formation and nuclear activity. They are predominantly located in isolated or small group environments, indicating that internal processes rather than external factors drive their quenching. Moreover, optical emission lines detected throughout a significant area of these systems suggest that gas depletion is unlikely to be the primary quenching mechanism. These findings support a scenario where quenching is instead caused by reduced star formation efficiency.","PeriodicalId":8585,"journal":{"name":"Astronomy & Astrophysics","volume":"30 8","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141800920","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}