Pub Date : 2025-03-21DOI: 10.1051/0004-6361/202451857
L. Zalesky, C. J. R. McPartland, J. R. Weaver, S. Toft, D. B. Sanders, B. Mobasher, N. Suzuki, I. Szapudi, I. Valdes, G. Murphree, N. Chartab, N. Allen, S. Taamoli, S. W. J. Barrow, O. Chávez Ortiz, S. L. Finkelstein, S. Gwyn, M. Sawicki, H. J. McCracken, D. Stern, H. Dannerbauer, B. Altieri, S. Andreon, N. Auricchio, C. Baccigalupi, M. Baldi, S. Bardelli, R. Bender, C. Bodendorf, D. Bonino, E. Branchini, M. Brescia, J. Brinchmann, S. Camera, V. Capobianco, C. Carbone, J. Carretero, S. Casas, F. J. Castander, M. Castellano, G. Castignani, S. Cavuoti, A. Cimatti, C. Colodro-Conde, G. Congedo, C. J. Conselice, L. Conversi, Y. Copin, L. Corcione, F. Courbin, H. M. Courtois, A. Da Silva, H. Degaudenzi, G. De Lucia, A. M. Di Giorgio, J. Dinis, F. Dubath, C. A. J. Duncan, X. Dupac, S. Dusini, M. Farina, S. Farrens, S. Ferriol, S. Fotopoulou, M. Frailis, E. Franceschi, S. Galeotta, B. Garilli, W. Gillard, B. Gillis, C. Giocoli, P. Gómez-Alvarez, A. Grazian, F. Grupp, S. V. H. Haugan, H. Hoekstra, W. Holmes, I. Hook, F. Hormuth, A. Hornstrup, P. Hudelot, K. Jahnke, B. Joachimi, E. Keihänen, S. Kermiche, A. Kiessling, M. Kilbinger, B. Kubik, K. Kuijken, M. Kümmel, M. Kunz, H. Kurki-Suonio, R. Laureijs, S. Ligori, P. B. Lilje, V. Lindholm, I. Lloro, G. Mainetti, D. Maino, E. Maiorano, O. Mansutti, O. Marggraf, K. Markovic, M. Martinelli, N. Martinet, F. Marulli, R. Massey, S. Maurogordato, S. Mei, Y. Mellier, M. Meneghetti, E. Merlin, G. Meylan, M. Moresco, L. Moscardini, E. Munari, C. Neissner, S.-M. Niemi, J. W. Nightingale, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, W. J. Percival, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L. A. Popa, L. Pozzetti, F. Raison, R. Rebolo, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, E. Rossetti, R. Saglia, Z. Sakr, D. Sapone, R. Scaramella, M. Schirmer, P. Schneider, T. Schrabback, A. Secroun, E. Sefusatti, G. Seidel, S. Serrano, C. Sirignano, G. Sirri, L. Stanco, J. Steinwagner, P. Tallada-Crespí, H. I. Teplitz, I. Tereno, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, E. A. Valentijn, L. Valenziano, T. Vassallo, G. Verdoes Kleijn, A. Veropalumbo, Y. Wang, J. Weller, G. Zamorani, E. Zucca, M. Bolzonella, A. Boucaud, E. Bozzo, C. Burigana, D. Di Ferdinando, J. A. Escartin Vigo, R. Farinelli, J. Gracia-Carpio, N. Mauri, A. A. Nucita, V. Scottez, M. Tenti, M. Viel, M. Wiesmann, Y. Akrami, V. Allevato, S. Anselmi, M. Ballardini, M. Bethermin, A. Blanchard, L. Blot, S. Borgani, S. Bruton, R. Cabanac, A. Calabro, A. Cappi, C. S. Carvalho, T. Castro, K. C. Chambers, R. Chary, S. Contarini, T. Contini, A. R. Cooray, B. De Caro, G. Desprez, A. Díaz-Sánchez, S. Di Domizio, H. Dole, S. Escoffier, A. G. Ferrari, I. Ferrero, F. Finelli, F. Fornari, L. Gabarra, K. Ganga, J. García-Bellido, E. Gaztanaga, F. Giacomini, G. Gozaliasl, A. Hall, W. G. Hartley, H. Hildebrandt, J. Hjorth, M. Huertas-Company, O. Ilbert, A. Jimenez Muñoz, J. J. E. Kajava, V. Kansal, D. Karagiannis, C. C. Kirkpatrick, L. Legrand, G. Libet, A. Loureiro, J. Macias-Perez, G. Maggio, M. Magliocchetti, C. Mancini, F. Mannucci, R. Maoli, C. J. A. P. Martins, S. Matthew, L. Maurin, R. B. Metcalf, P. Monaco, C. Moretti, G. Morgante, Nicholas A. Walton, J. Odier, L. Patrizii, A. Pezzotta, M. Pöntinen, V. Popa, C. Porciani, D. Potter, P. Reimberg, I. Risso, P.-F. Rocci, M. Sahlén, C. Scarlata, A. Schneider, M. Sereno, A. Silvestri, P. Simon, A. Spurio Mancini, S. A. Stanford, C. Tao, G. Testera, R. Teyssier, S. Tosi, A. Troja, M. Tucci, C. Valieri, J. Valiviita, D. Vergani, G. Verza, I. A. Zinchenko
The Cosmic Dawn Survey (DAWN survey) provides multiwavelength (UV/optical to mid-IR) data across the combined 59 deg2 of the Euclid Deep and Auxiliary fields (EDFs and EAFs). In this work, the first public data release from the DAWN survey is presented. The catalogues made available herein consist of a subset of the full DAWN survey that includes two EDFs: EDF North (EDF-N) and EDF Fornax (EDF-F). Each field has been covered by the ongoing Hawaii Twenty Square Degree Survey (H20), which includes imaging from the CFHT MegaCam in the u filter and from the Subaru Hyper Suprime-Cam (HSC) in the griz filters. Each field has been further covered by Spitzer/IRAC 3.6–4.5µm imaging spanning 10 deg2 and reaching ~25 mag AB (5σ). All present H20 imaging and all publicly available imaging from the aforementioned facilities were combined with the deep Spitzer/IRAC data to create source catalogues spanning a total area of 16.87 deg2 in EDF-N and 2.85 deg2 in EDF-F for this first release. These catalogues are referred to as the ‘pre-launch’ (PL), as Euclid data is not yet public for these fields and therefore it is not included. Photometry was measured from these multiwavelength data using The Farmer, a novel and well validated model-based photometry code. Photometric redshifts and stellar masses were computed using two independent codes for modelling spectral energy distributions: EAZY and LePhare. Photometric redshifts show good agreement with spectroscopic redshifts (σNMAD ~ 0.5, η < 8% at i < 25). Number counts, photometric redshifts and stellar masses were further validated in comparison to the COSMOS2020 catalogue. The DAWN survey PL catalogues are designed to be of immediate use in these two EDFs and will be continuously updated and made available as both new ground-based data and spaced-based data from Euclid are acquired and made public. Future data releases will provide catalogues of all EDFs and EAFs and include Euclid data.
{"title":"Euclid preparation","authors":"L. Zalesky, C. J. R. McPartland, J. R. Weaver, S. Toft, D. B. Sanders, B. Mobasher, N. Suzuki, I. Szapudi, I. Valdes, G. Murphree, N. Chartab, N. Allen, S. Taamoli, S. W. J. Barrow, O. Chávez Ortiz, S. L. Finkelstein, S. Gwyn, M. Sawicki, H. J. McCracken, D. Stern, H. Dannerbauer, B. Altieri, S. Andreon, N. Auricchio, C. Baccigalupi, M. Baldi, S. Bardelli, R. Bender, C. Bodendorf, D. Bonino, E. Branchini, M. Brescia, J. Brinchmann, S. Camera, V. Capobianco, C. Carbone, J. Carretero, S. Casas, F. J. Castander, M. Castellano, G. Castignani, S. Cavuoti, A. Cimatti, C. Colodro-Conde, G. Congedo, C. J. Conselice, L. Conversi, Y. Copin, L. Corcione, F. Courbin, H. M. Courtois, A. Da Silva, H. Degaudenzi, G. De Lucia, A. M. Di Giorgio, J. Dinis, F. Dubath, C. A. J. Duncan, X. Dupac, S. Dusini, M. Farina, S. Farrens, S. Ferriol, S. Fotopoulou, M. Frailis, E. Franceschi, S. Galeotta, B. Garilli, W. Gillard, B. Gillis, C. Giocoli, P. Gómez-Alvarez, A. Grazian, F. Grupp, S. V. H. Haugan, H. Hoekstra, W. Holmes, I. Hook, F. Hormuth, A. Hornstrup, P. Hudelot, K. Jahnke, B. Joachimi, E. Keihänen, S. Kermiche, A. Kiessling, M. Kilbinger, B. Kubik, K. Kuijken, M. Kümmel, M. Kunz, H. Kurki-Suonio, R. Laureijs, S. Ligori, P. B. Lilje, V. Lindholm, I. Lloro, G. Mainetti, D. Maino, E. Maiorano, O. Mansutti, O. Marggraf, K. Markovic, M. Martinelli, N. Martinet, F. Marulli, R. Massey, S. Maurogordato, S. Mei, Y. Mellier, M. Meneghetti, E. Merlin, G. Meylan, M. Moresco, L. Moscardini, E. Munari, C. Neissner, S.-M. Niemi, J. W. Nightingale, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, W. J. Percival, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L. A. Popa, L. Pozzetti, F. Raison, R. Rebolo, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, E. Rossetti, R. Saglia, Z. Sakr, D. Sapone, R. Scaramella, M. Schirmer, P. Schneider, T. Schrabback, A. Secroun, E. Sefusatti, G. Seidel, S. Serrano, C. Sirignano, G. Sirri, L. Stanco, J. Steinwagner, P. Tallada-Crespí, H. I. Teplitz, I. Tereno, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, E. A. Valentijn, L. Valenziano, T. Vassallo, G. Verdoes Kleijn, A. Veropalumbo, Y. Wang, J. Weller, G. Zamorani, E. Zucca, M. Bolzonella, A. Boucaud, E. Bozzo, C. Burigana, D. Di Ferdinando, J. A. Escartin Vigo, R. Farinelli, J. Gracia-Carpio, N. Mauri, A. A. Nucita, V. Scottez, M. Tenti, M. Viel, M. Wiesmann, Y. Akrami, V. Allevato, S. Anselmi, M. Ballardini, M. Bethermin, A. Blanchard, L. Blot, S. Borgani, S. Bruton, R. Cabanac, A. Calabro, A. Cappi, C. S. Carvalho, T. Castro, K. C. Chambers, R. Chary, S. Contarini, T. Contini, A. R. Cooray, B. De Caro, G. Desprez, A. Díaz-Sánchez, S. Di Domizio, H. Dole, S. Escoffier, A. G. Ferrari, I. Ferrero, F. Finelli, F. Fornari, L. Gabarra, K. Ganga, J. García-Bellido, E. Gaztanaga, F. Giacomini, G. Gozaliasl, A. Hall, W. G. Hartley, H. Hildebrandt, J. Hjorth, M. Huertas-Company, O. Ilbert, A. Jimenez Muñoz, J. J. E. Kajava, V. Kansal, D. Karagiannis, C. C. Kirkpatrick, L. Legrand, G. Libet, A. Loureiro, J. Macias-Perez, G. Maggio, M. Magliocchetti, C. Mancini, F. Mannucci, R. Maoli, C. J. A. P. Martins, S. Matthew, L. Maurin, R. B. Metcalf, P. Monaco, C. Moretti, G. Morgante, Nicholas A. Walton, J. Odier, L. Patrizii, A. Pezzotta, M. Pöntinen, V. Popa, C. Porciani, D. Potter, P. Reimberg, I. Risso, P.-F. Rocci, M. Sahlén, C. Scarlata, A. Schneider, M. Sereno, A. Silvestri, P. Simon, A. Spurio Mancini, S. A. Stanford, C. Tao, G. Testera, R. Teyssier, S. Tosi, A. Troja, M. Tucci, C. Valieri, J. Valiviita, D. Vergani, G. Verza, I. A. Zinchenko","doi":"10.1051/0004-6361/202451857","DOIUrl":"https://doi.org/10.1051/0004-6361/202451857","url":null,"abstract":"The Cosmic Dawn Survey (DAWN survey) provides multiwavelength (UV/optical to mid-IR) data across the combined 59 deg<sup>2<sup/> of the Euclid Deep and Auxiliary fields (EDFs and EAFs). In this work, the first public data release from the DAWN survey is presented. The catalogues made available herein consist of a subset of the full DAWN survey that includes two EDFs: EDF North (EDF-N) and EDF Fornax (EDF-F). Each field has been covered by the ongoing Hawaii Twenty Square Degree Survey (H20), which includes imaging from the CFHT MegaCam in the <i>u<i/> filter and from the Subaru Hyper Suprime-Cam (HSC) in the <i>griz<i/> filters. Each field has been further covered by <i>Spitzer<i/>/IRAC 3.6–4.5µm imaging spanning 10 deg<sup>2<sup/> and reaching ~25 mag AB (5<i>σ<i/>). All present H20 imaging and all publicly available imaging from the aforementioned facilities were combined with the deep <i>Spitzer<i/>/IRAC data to create source catalogues spanning a total area of 16.87 deg<sup>2<sup/> in EDF-N and 2.85 deg<sup>2<sup/> in EDF-F for this first release. These catalogues are referred to as the ‘pre-launch’ (PL), as <i>Euclid<i/> data is not yet public for these fields and therefore it is not included. Photometry was measured from these multiwavelength data using The Farmer, a novel and well validated model-based photometry code. Photometric redshifts and stellar masses were computed using two independent codes for modelling spectral energy distributions: EAZY and LePhare. Photometric redshifts show good agreement with spectroscopic redshifts (<i>σ<i/><sub>NMAD<sub/> ~ 0.5, <i>η <<i/> 8% at <i>i<i/> < 25). Number counts, photometric redshifts and stellar masses were further validated in comparison to the COSMOS2020 catalogue. The DAWN survey PL catalogues are designed to be of immediate use in these two EDFs and will be continuously updated and made available as both new ground-based data and spaced-based data from <i>Euclid<i/> are acquired and made public. Future data releases will provide catalogues of all EDFs and EAFs and include <i>Euclid<i/> data.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"57 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677762","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-21DOI: 10.1051/0004-6361/202452924
J. W. Zhou, Pavel Kroupa, Sami Dib
Many studies have revealed that the core mass function (CMF) in high-mass star-forming regions is top-heavy. In this work, we start from the canonical initial mass function (IMF) to inversely synthesize the observed CMFs of high-mass star formation regions, taking into account variations in multiplicity and mass conversion efficiency from core to star (ϵcore). To match the observed CMFs, cores of different masses should have varying ϵcore, with ϵcore increasing as the core mass decreases. However, the multiplicity fraction does not affect the synthesized CMFs. To accurately fit the high-mass end of the CMF, it is essential to determine whether the CMF shows a slope transition from the low-mass end to the high-mass one. If the CMF truly undergoes a slope transition but observational biases obscure it, leading to a combined fit with a shallower slope, this could artificially create a top-heavy CMF.
{"title":"Inversely synthesizing the core mass function of high-mass star-forming regions from the canonical initial mass function","authors":"J. W. Zhou, Pavel Kroupa, Sami Dib","doi":"10.1051/0004-6361/202452924","DOIUrl":"https://doi.org/10.1051/0004-6361/202452924","url":null,"abstract":"Many studies have revealed that the core mass function (CMF) in high-mass star-forming regions is top-heavy. In this work, we start from the canonical initial mass function (IMF) to inversely synthesize the observed CMFs of high-mass star formation regions, taking into account variations in multiplicity and mass conversion efficiency from core to star (<i>ϵ<i/><sub>core<sub/>). To match the observed CMFs, cores of different masses should have varying <i>ϵ<i/><sub>core<sub/>, with <i>ϵ<i/><sub>core<sub/> increasing as the core mass decreases. However, the multiplicity fraction does not affect the synthesized CMFs. To accurately fit the high-mass end of the CMF, it is essential to determine whether the CMF shows a slope transition from the low-mass end to the high-mass one. If the CMF truly undergoes a slope transition but observational biases obscure it, leading to a combined fit with a shallower slope, this could artificially create a top-heavy CMF.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"26 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677763","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-21DOI: 10.1051/0004-6361/202453279
Romain A. Meyer, Fabian Walter, Fabio Di Mascia, Roberto Decarli, Marcel Neeleman, Bram Venemans
The temperature of the cold dust in z > 6 galaxies is a potential tracer of the presence of an active galactic nucleus (AGN) and stellar feedback. This is also the dominant source of uncertainty in inferring properties from the far-infrared (FIR) emission of these galaxies. We present the first resolved dust temperature map in a z > 6 quasar host galaxy. We combined new 360 parsec (pc) resolution ALMA Band 9 continuum observations with 190 pc Band 6 observations from the literature to derive the dust temperature and opacity at 0.1 < r < 0.5 kpc scales in a z = 6.9 luminous quasar host galaxy (J2348–3054). We find that the dust temperature (and opacity) increases at the center (r < 216 pc) of the galaxy up to Td = 73 − 88 K, potentially rising up to Td < 149 K at r < 110 pc. The combination of the resolved and integrated FIR spectral energy distribution (SED) further reveal a dust temperature gradient and a significant contribution of the AGN hot dust torus at νobs ≳ 700 GHz. By taking into account the torus contribution and resolved optically thick emission, we derived the total IR luminosity (LTIR = 8.78 ± 0.10) × 1012L⊙) and corresponding star formation rate (SFR = 1307 ± 15 M⊙yr-1), which are at least a factor of ∼3.6 (∼0.56 dex) lower than previous measurements based on the assumption of optically thin emission. We compared the resolved dust temperature, mass, and IR luminosity profiles to simulations where they are only reproduced by models that include the AGN radiation heating the dust in the center of the galaxy. Our observations provide evidence that dust in J2348–3054 cannot be assumed to be uniformly cold and optically thin. Whether J2348–3054 is representative of the larger population of high-redshift quasars and galaxies remains to be determined with future dedicated high-resolution and high-frequency ALMA observations.
{"title":"ALMA 360 parsec, high-frequency observations reveal warm dust in the center of a z = 6.9 quasar","authors":"Romain A. Meyer, Fabian Walter, Fabio Di Mascia, Roberto Decarli, Marcel Neeleman, Bram Venemans","doi":"10.1051/0004-6361/202453279","DOIUrl":"https://doi.org/10.1051/0004-6361/202453279","url":null,"abstract":"The temperature of the cold dust in <i>z<i/> > 6 galaxies is a potential tracer of the presence of an active galactic nucleus (AGN) and stellar feedback. This is also the dominant source of uncertainty in inferring properties from the far-infrared (FIR) emission of these galaxies. We present the first resolved dust temperature map in a <i>z<i/> > 6 quasar host galaxy. We combined new 360 parsec (pc) resolution ALMA Band 9 continuum observations with 190 pc Band 6 observations from the literature to derive the dust temperature and opacity at 0.1 < <i>r<i/> < 0.5 kpc scales in a <i>z<i/> = 6.9 luminous quasar host galaxy (J2348–3054). We find that the dust temperature (and opacity) increases at the center (<i>r<i/> < 216 pc) of the galaxy up to <i>T<sub>d<sub/><i/> = 73 − 88 K, potentially rising up to <i>T<sub>d<sub/><i/> < 149 K at <i>r<i/> < 110 pc. The combination of the resolved and integrated FIR spectral energy distribution (SED) further reveal a dust temperature gradient and a significant contribution of the AGN hot dust torus at ν<sub>obs<sub/> ≳ 700 GHz. By taking into account the torus contribution and resolved optically thick emission, we derived the total IR luminosity (<i>L<i/><sub>TIR<sub/> = 8.78 ± 0.10) × 10<sup>12<sup/> <i>L<i/><sub>⊙<sub/>) and corresponding star formation rate (SFR = 1307 ± 15 <i>M<i/><sub>⊙<sub/>yr<sup>-1<sup/>), which are at least a factor of ∼3.6 (∼0.56 dex) lower than previous measurements based on the assumption of optically thin emission. We compared the resolved dust temperature, mass, and IR luminosity profiles to simulations where they are only reproduced by models that include the AGN radiation heating the dust in the center of the galaxy. Our observations provide evidence that dust in J2348–3054 cannot be assumed to be uniformly cold and optically thin. Whether J2348–3054 is representative of the larger population of high-redshift quasars and galaxies remains to be determined with future dedicated high-resolution and high-frequency ALMA observations.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"94 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677765","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-20DOI: 10.1051/0004-6361/202452627
X. Xu, R. F. Peletier, P. Awad, M. A. Raj, R. Smith
<i>Context.<i/> Dwarf galaxies play an important role when studying the effects of the environment on galaxy formation and evolution. The Fornax cluster, having a dense core and strong tidal fields, offers an ideal laboratory for investigating the influence of the cluster environment on the morphology of dwarf galaxies.<i>Aims.<i/> We explore the relationship between the morphology of galaxies, in particular the asymmetries, and their distances to the cluster centre to study the effect of tidal forces and other environmental processes. We did this by investigating the detailed morphologies of a complete magnitude-limited sample of 556 galaxies within the Fornax cluster, spanning a radius range up to 1.75 Mpc from its central to the outer regions.<i>Methods.<i/> For galaxies in the Fornax Deep Survey, we quantified the morphologies of dwarf galaxies using the non-parametric quantities asymmetry (<i>A<i/>) and smoothness (<i>S<i/>), as part of the CAS system. Unlike previous work, we used isophotal CAS parameters, which are sensitive to the outer parts of galaxies. We constructed <i>A<i/> − <i>r<i/> (asymmetry vs. distance to cluster centre) and <i>S<i/> − <i>r<i/> (smoothness vs. distance to the cluster centre) diagrams to investigate the relationship between morphology and distance. Additionally, we examined the effects of asymmetry on magnitude and colour. Furthermore, to better understand the assembly history of the galaxy cluster, we performed a phase-space analysis for Fornax dwarf galaxies, using spectroscopic redshifts and the projected distance from the cluster centre.<i>Results.<i/> We find that dwarf galaxies in the outer regions of the Fornax cluster have higher values of asymmetry compared to other dwarfs in the cluster, indicating a greater degree of morphological disturbances within dwarf galaxies in these regions. We also find that galaxies in the very inner regions are more asymmetric than those farther out. The <i>A<i/>-magnitude relation reveals a trend where asymmetry increases as galaxies become fainter, and the <i>A<i/>-colour relation shows that galaxies with bluer colours tend to exhibit stronger asymmetry. We do not find any correlations with smoothness, except that smoothness strongly decreases with stellar mass. We propose that the higher asymmetry of dwarfs in the outer regions is most likely caused by ram pressure stripping. As galaxies fall into the cluster, gas is expelled by intracluster winds, causing ‘jellyfish-like’ tails and leading to star formation not only in the central regions but also along the tails; this causes the asymmetric features. These asymmetries persist until the galaxies evolve into completely quiescent and elliptical systems. The observed dwarfs likely represent a transitional phase, during which they are nearing quiescence but still retain residual asymmetry from earlier interactions. In the very inner parts, the asymmetries most likely are caused by tidal effects. In addition, our phase-space
{"title":"Asymmetry at low surface brightnesses as an indicator of environmental processes in the Fornax cluster","authors":"X. Xu, R. F. Peletier, P. Awad, M. A. Raj, R. Smith","doi":"10.1051/0004-6361/202452627","DOIUrl":"https://doi.org/10.1051/0004-6361/202452627","url":null,"abstract":"<i>Context.<i/> Dwarf galaxies play an important role when studying the effects of the environment on galaxy formation and evolution. The Fornax cluster, having a dense core and strong tidal fields, offers an ideal laboratory for investigating the influence of the cluster environment on the morphology of dwarf galaxies.<i>Aims.<i/> We explore the relationship between the morphology of galaxies, in particular the asymmetries, and their distances to the cluster centre to study the effect of tidal forces and other environmental processes. We did this by investigating the detailed morphologies of a complete magnitude-limited sample of 556 galaxies within the Fornax cluster, spanning a radius range up to 1.75 Mpc from its central to the outer regions.<i>Methods.<i/> For galaxies in the Fornax Deep Survey, we quantified the morphologies of dwarf galaxies using the non-parametric quantities asymmetry (<i>A<i/>) and smoothness (<i>S<i/>), as part of the CAS system. Unlike previous work, we used isophotal CAS parameters, which are sensitive to the outer parts of galaxies. We constructed <i>A<i/> − <i>r<i/> (asymmetry vs. distance to cluster centre) and <i>S<i/> − <i>r<i/> (smoothness vs. distance to the cluster centre) diagrams to investigate the relationship between morphology and distance. Additionally, we examined the effects of asymmetry on magnitude and colour. Furthermore, to better understand the assembly history of the galaxy cluster, we performed a phase-space analysis for Fornax dwarf galaxies, using spectroscopic redshifts and the projected distance from the cluster centre.<i>Results.<i/> We find that dwarf galaxies in the outer regions of the Fornax cluster have higher values of asymmetry compared to other dwarfs in the cluster, indicating a greater degree of morphological disturbances within dwarf galaxies in these regions. We also find that galaxies in the very inner regions are more asymmetric than those farther out. The <i>A<i/>-magnitude relation reveals a trend where asymmetry increases as galaxies become fainter, and the <i>A<i/>-colour relation shows that galaxies with bluer colours tend to exhibit stronger asymmetry. We do not find any correlations with smoothness, except that smoothness strongly decreases with stellar mass. We propose that the higher asymmetry of dwarfs in the outer regions is most likely caused by ram pressure stripping. As galaxies fall into the cluster, gas is expelled by intracluster winds, causing ‘jellyfish-like’ tails and leading to star formation not only in the central regions but also along the tails; this causes the asymmetric features. These asymmetries persist until the galaxies evolve into completely quiescent and elliptical systems. The observed dwarfs likely represent a transitional phase, during which they are nearing quiescence but still retain residual asymmetry from earlier interactions. In the very inner parts, the asymmetries most likely are caused by tidal effects. In addition, our phase-space ","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"183 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143666080","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-20DOI: 10.1051/0004-6361/202452286
Hugo Tranin, Nadejda Blagorodnova, Viraj Karambelkar, Paul J. Groot, Steven Bloemen, Paul M. Vreeswijk, Daniëlle L. A. Pieterse, Jan van Roestel
Context. After the main sequence phase, stars more massive than 2.5 M⊙ rapidly evolve through the Hertzsprung gap as yellow giants and yellow supergiants (YSGs) before settling into the red giant branch. Identifying Hertzsprung gap stars in nearby galaxies is crucial for pinpointing progenitors of luminous red novae (LRNe) – astrophysical transients attributed to stellar mergers. In the era of extensive transient surveys like the Vera C. Rubin Observatory’s Legacy Survey of Space and Time (LSST), this approach offers a new way to predict and select common envelope transients.Aims. This study investigates potential progenitors and precursors of LRNe by analysing Hubble Space Telescope (HST) photometry of stellar populations in galaxies within ∼20 Mpc to identify YSG candidates. Additionally, we use the Zwicky Transient Facility and MeerLICHT/BlackGEM to identify possible precursors, preparing for future observations by the LSST.Methods. We compiled a sample of 369 galaxies with HST exposures in the F 475W, F 555W, F 606W, and F814W filters. We identified YSG candidates using MESA stellar evolution tracks and statistical analysis of colour–magnitude diagrams.Results. Our sample includes 154 494 YSG candidates with masses between 3 M⊙ and 20 M⊙ and is affected by various contaminants, notably foreground stars and extinguished main sequence stars. After excluding foreground stars using Gaia proper motions, contamination is estimated at 1% from foreground stars (based on TRILEGAL simulations) and ∼20% from extinction affecting main sequence stars. Combining our YSG candidates with time-domain catalogues yielded several interesting candidates. In particular, we identified 12 LRN precursor candidates for which follow-up is encouraged.Conclusions. We highlight the importance of monitoring future transients that match YSG candidates to avoid missing potential LRNe and other rare transients. LSST will be a game changer in the search for LRN progenitors and precursors; it is predicted to discover over 300 000 new YSG candidates and 100 LRN precursors within 20 Mpc.
{"title":"Hertzsprung gap stars in nearby galaxies and the quest for luminous red nova progenitors","authors":"Hugo Tranin, Nadejda Blagorodnova, Viraj Karambelkar, Paul J. Groot, Steven Bloemen, Paul M. Vreeswijk, Daniëlle L. A. Pieterse, Jan van Roestel","doi":"10.1051/0004-6361/202452286","DOIUrl":"https://doi.org/10.1051/0004-6361/202452286","url":null,"abstract":"<i>Context.<i/> After the main sequence phase, stars more massive than 2.5 M<sub>⊙<sub/> rapidly evolve through the Hertzsprung gap as yellow giants and yellow supergiants (YSGs) before settling into the red giant branch. Identifying Hertzsprung gap stars in nearby galaxies is crucial for pinpointing progenitors of luminous red novae (LRNe) – astrophysical transients attributed to stellar mergers. In the era of extensive transient surveys like the <i>Vera C. Rubin<i/> Observatory’s Legacy Survey of Space and Time (LSST), this approach offers a new way to predict and select common envelope transients.<i>Aims.<i/> This study investigates potential progenitors and precursors of LRNe by analysing <i>Hubble<i/> Space Telescope (HST) photometry of stellar populations in galaxies within ∼20 Mpc to identify YSG candidates. Additionally, we use the <i>Zwicky<i/> Transient Facility and MeerLICHT/BlackGEM to identify possible precursors, preparing for future observations by the LSST.<i>Methods.<i/> We compiled a sample of 369 galaxies with HST exposures in the <i>F<i/> 475<i>W<i/>, <i>F<i/> 555<i>W<i/>, <i>F<i/> 606<i>W<i/>, and <i>F<i/>814<i>W<i/> filters. We identified YSG candidates using MESA stellar evolution tracks and statistical analysis of colour–magnitude diagrams.<i>Results.<i/> Our sample includes 154 494 YSG candidates with masses between 3 <i>M<i/><sub>⊙<sub/> and 20 <i>M<i/><sub>⊙<sub/> and is affected by various contaminants, notably foreground stars and extinguished main sequence stars. After excluding foreground stars using <i>Gaia<i/> proper motions, contamination is estimated at 1% from foreground stars (based on TRILEGAL simulations) and ∼20% from extinction affecting main sequence stars. Combining our YSG candidates with time-domain catalogues yielded several interesting candidates. In particular, we identified 12 LRN precursor candidates for which follow-up is encouraged.<i>Conclusions.<i/> We highlight the importance of monitoring future transients that match YSG candidates to avoid missing potential LRNe and other rare transients. LSST will be a game changer in the search for LRN progenitors and precursors; it is predicted to discover over 300 000 new YSG candidates and 100 LRN precursors within 20 Mpc.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"199 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143666083","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-20DOI: 10.1051/0004-6361/202452209
Silvio Rodríguez, Valeria A. Cristiani, Laura V. Sales, Mario G. Abadi
Context. Disc-dominated galaxies can be difficult to accommodate in a hierarchical formation scenario such as Λ cold dark matter (ΛCDM), where mergers are an important growth mechanism. However, observational evidence indicates that these galaxies are common in the Universe.Aims. We seek to characterise the conditions that lead to the formation of disc-dominated galaxies within ΛCDM.Methods. We used dynamical decomposition of the stellar particles in all galaxies with stellar mass M∗ = [1010 − 1011] M⊙ within the cosmological hydrodynamical simulation Illustris TNG100. We selected a sample of 43 mostly-disc galaxies that have less than ∼10% of their mass in a bulge component. For comparison, we also studied two additional stellar-mass matched samples: 43 intermediate galaxies having ∼30% of their stellar mass in the bulge and 43 with a purely spheroidal-like morphology.Results. We find that the selection purely based on stellar dynamics is able to reproduce the expected stellar population trends of different morphological types, with higher star-formation rates and younger stars in disc-dominated galaxies. Halo spin seems to play no role in the morphology of the galaxies, in agreement with previous works. At a fixed M*, our mostly-disc and intermediate samples form in dark matter haloes that are two to ten times less massive than the spheroidal sample, highlighting a higher efficiency in disc galaxies to retain and condensate their baryons. On average, mergers are less prevalent in the buildup of discs than in spheroidal galaxies, but there is a large scatter, including the existence of mostly-disc galaxies, with 15%–30% of their stars coming from accreted origin. Discs start to form early on, settling their low vertical velocity dispersion as early as 9–10 Gyr ago, although the dominance of the disc over the spheroid was established more recently (3–4 Gyr lookback time). The most rotationally supported discs form in haloes with the lowest virial mass in the sample and the best aligned distribution of angular momentum in the gas.
{"title":"The assembly of the most rotationally supported disc galaxies in the TNG100 simulations","authors":"Silvio Rodríguez, Valeria A. Cristiani, Laura V. Sales, Mario G. Abadi","doi":"10.1051/0004-6361/202452209","DOIUrl":"https://doi.org/10.1051/0004-6361/202452209","url":null,"abstract":"<i>Context.<i/> Disc-dominated galaxies can be difficult to accommodate in a hierarchical formation scenario such as Λ cold dark matter (ΛCDM), where mergers are an important growth mechanism. However, observational evidence indicates that these galaxies are common in the Universe.<i>Aims.<i/> We seek to characterise the conditions that lead to the formation of disc-dominated galaxies within ΛCDM.<i>Methods.<i/> We used dynamical decomposition of the stellar particles in all galaxies with stellar mass <i>M<i/><sub>∗<sub/> = [10<sup>10<sup/> − 10<sup>11<sup/>] M<sub>⊙<sub/> within the cosmological hydrodynamical simulation Illustris TNG100. We selected a sample of 43 mostly-disc galaxies that have less than ∼10% of their mass in a bulge component. For comparison, we also studied two additional stellar-mass matched samples: 43 intermediate galaxies having ∼30% of their stellar mass in the bulge and 43 with a purely spheroidal-like morphology.<i>Results.<i/> We find that the selection purely based on stellar dynamics is able to reproduce the expected stellar population trends of different morphological types, with higher star-formation rates and younger stars in disc-dominated galaxies. Halo spin seems to play no role in the morphology of the galaxies, in agreement with previous works. At a fixed <i>M<i/><sub>*<sub/>, our mostly-disc and intermediate samples form in dark matter haloes that are two to ten times less massive than the spheroidal sample, highlighting a higher efficiency in disc galaxies to retain and condensate their baryons. On average, mergers are less prevalent in the buildup of discs than in spheroidal galaxies, but there is a large scatter, including the existence of mostly-disc galaxies, with 15%–30% of their stars coming from accreted origin. Discs start to form early on, settling their low vertical velocity dispersion as early as 9–10 Gyr ago, although the dominance of the disc over the spheroid was established more recently (3–4 Gyr lookback time). The most rotationally supported discs form in haloes with the lowest virial mass in the sample and the best aligned distribution of angular momentum in the gas.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"27 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143666079","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-20DOI: 10.1051/0004-6361/202449599
F. Kleinebreil, S. Grandis, T. Schrabback, V. Ghirardini, I. Chiu, A. Liu, M. Kluge, T. H. Reiprich, E. Artis, Y. E. Bahar, F. Balzer, E. Bulbul, N. Clerc, J. Comparat, C. Garrel, D. Gruen, X. Li, H. Miyatake, S. Miyazaki, M. E. Ramos-Ceja, J. Sanders, R. Seppi, N. Okabe, X. Zhang
Aims. We aim to participate in the calibration of the X-ray photon count rate to halo mass scaling relation of galaxy clusters selected in the first eROSITA All-Sky Survey on the western Galactic hemisphere (eRASS1) using weak-lensing (WL) data from the fourth data release of the Kilo-Degree Survey (KiDS-1000). We therefore measured the radial shear profiles around eRASS1 galaxy clusters using background galaxies in KiDS-1000 as well as the cluster member contamination. Furthermore, we provide consistency checks with the other stage-III weak-lensing surveys that take part in the eRASS1 mass calibration, the Dark Energy Survey Year 3 (DES Y3) and Hyper Suprime-Cam Year 3 (HSC-Y3), as KiDS-1000 has overlap with both surveys.Methods. We determined the cluster member contamination of eRASS1 clusters present in KiDS-1000 based on background galaxy number density profiles, where we accounted for the optical obscuration caused by cluster galaxies. The extracted shear profiles, together with the result of the contamination model and the lens sample selection, were then analysed through a Bayesian population model. We calibrated the WL mass bias parameter by analysing realistic synthetic shear profiles from mock cluster catalogues. Our consistency checks between KiDS-1000 and DES Y3 and HSC-Y3 include the comparison of contamination-corrected density contrast profiles and amplitudes by employing the union of background sources around common clusters as well as the individual scaling relation results.Results. We present a global contamination model for eRASS1 clusters in KiDS-1000 and the calibration results of the X-ray photon count rate to halo mass relation. The results of the WL mass bias parameter bWL obtained through mock observations show that hydro-dynamical modelling uncertainties only play a sub-dominant role in KiDS-1000. The uncertainty of the multiplicative shear bias dominates the systematic error budget at low cluster redshifts, while the uncertainty of our contamination model does so at high ones. The crosschecks between the three WL surveys show that they are for the most part statistically consistent with each other. This enables, for the first time, cosmological constraints from clusters calibrated by three state-of-the-art weak-lensing surveys.
{"title":"The SRG/eROSITA All-Sky Survey","authors":"F. Kleinebreil, S. Grandis, T. Schrabback, V. Ghirardini, I. Chiu, A. Liu, M. Kluge, T. H. Reiprich, E. Artis, Y. E. Bahar, F. Balzer, E. Bulbul, N. Clerc, J. Comparat, C. Garrel, D. Gruen, X. Li, H. Miyatake, S. Miyazaki, M. E. Ramos-Ceja, J. Sanders, R. Seppi, N. Okabe, X. Zhang","doi":"10.1051/0004-6361/202449599","DOIUrl":"https://doi.org/10.1051/0004-6361/202449599","url":null,"abstract":"<i>Aims.<i/> We aim to participate in the calibration of the X-ray photon count rate to halo mass scaling relation of galaxy clusters selected in the first eROSITA All-Sky Survey on the western Galactic hemisphere (eRASS1) using weak-lensing (WL) data from the fourth data release of the Kilo-Degree Survey (KiDS-1000). We therefore measured the radial shear profiles around eRASS1 galaxy clusters using background galaxies in KiDS-1000 as well as the cluster member contamination. Furthermore, we provide consistency checks with the other stage-III weak-lensing surveys that take part in the eRASS1 mass calibration, the Dark Energy Survey Year 3 (DES Y3) and Hyper Suprime-Cam Year 3 (HSC-Y3), as KiDS-1000 has overlap with both surveys.<i>Methods.<i/> We determined the cluster member contamination of eRASS1 clusters present in KiDS-1000 based on background galaxy number density profiles, where we accounted for the optical obscuration caused by cluster galaxies. The extracted shear profiles, together with the result of the contamination model and the lens sample selection, were then analysed through a Bayesian population model. We calibrated the WL mass bias parameter by analysing realistic synthetic shear profiles from mock cluster catalogues. Our consistency checks between KiDS-1000 and DES Y3 and HSC-Y3 include the comparison of contamination-corrected density contrast profiles and amplitudes by employing the union of background sources around common clusters as well as the individual scaling relation results.<i>Results.<i/> We present a global contamination model for eRASS1 clusters in KiDS-1000 and the calibration results of the X-ray photon count rate to halo mass relation. The results of the WL mass bias parameter <i>b<i/><sub>WL<sub/> obtained through mock observations show that hydro-dynamical modelling uncertainties only play a sub-dominant role in KiDS-1000. The uncertainty of the multiplicative shear bias dominates the systematic error budget at low cluster redshifts, while the uncertainty of our contamination model does so at high ones. The crosschecks between the three WL surveys show that they are for the most part statistically consistent with each other. This enables, for the first time, cosmological constraints from clusters calibrated by three state-of-the-art weak-lensing surveys.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"92 6 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143665912","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-20DOI: 10.1051/0004-6361/202451366
V. M. A. Gómez-González, L. M. Oskinova, W.-R. Hamann, H. Todt, D. Pauli, S. Reyero Serantes, M. Bernini-Peron, A. A. C. Sander, V. Ramachandran, J. S. Vink, P. A. Crowther, S. R. Berlanas, A. ud-Doula, A. C. Gormaz-Matamala, C. Kehrig, R. Kuiper, C. Leitherer, L. Mahy, A. F. McLeod, A. Mehner, N. Morrell, T. Shenar, O. G. Telford, J. Th. van Loon, F. Tramper, A. Wofford
Massive stars drive the ionization and mechanical feedback within young star-forming regions. The Large Magellanic Cloud (LMC) is an ideal galaxy for studying individual massive stars and quantifying their feedback contribution to the environment. We analyze eight exemplary targets in LMC N11 B from the Hubble UV Legacy Library of Young Stars as Essential Standards (ULLYSES) program using novel spectra from HST (COS and STIS) in the UV, and from VLT (X-shooter) in the optical. We model the spectra of early to late O-type stars using state-of-the-art PoWR atmosphere models. We determine the stellar and wind parameters (e.g., T⋆, log g, L⋆, Ṁ, and v∞) of the analyzed objects, chemical abundances (C, N, and O), ionizing and mechanical feedback (QH, QHeI, QHe II, and Lmec), and X-rays. We report ages of 2–4.5 Myr and masses of 30–60 M⊙ for the analyzed stars in N11 B, which are consistent with a scenario of sequential star formation. We note that the observed wind-momentum–luminosity relation is consistent with theoretical predictions. We detect nitrogen enrichment by up to a factor of seven in most of the stars. However, we do not find a correlation between nitrogen enrichment and projected rotational velocity. Finally, based on their spectral type, we estimate the total ionizing photons injected from the O-type stars in N11 B into its environment. We report log (Σ QH) = 50.5 ph s−1, log (Σ QHe I) = 49.6 ph s−1, and log (Σ QHe II)= 44.4 ph s−1, consistent with the total ionizing budget in N11.
{"title":"X-Shooting ULLYSES: Massive stars at low metallicity","authors":"V. M. A. Gómez-González, L. M. Oskinova, W.-R. Hamann, H. Todt, D. Pauli, S. Reyero Serantes, M. Bernini-Peron, A. A. C. Sander, V. Ramachandran, J. S. Vink, P. A. Crowther, S. R. Berlanas, A. ud-Doula, A. C. Gormaz-Matamala, C. Kehrig, R. Kuiper, C. Leitherer, L. Mahy, A. F. McLeod, A. Mehner, N. Morrell, T. Shenar, O. G. Telford, J. Th. van Loon, F. Tramper, A. Wofford","doi":"10.1051/0004-6361/202451366","DOIUrl":"https://doi.org/10.1051/0004-6361/202451366","url":null,"abstract":"Massive stars drive the ionization and mechanical feedback within young star-forming regions. The Large Magellanic Cloud (LMC) is an ideal galaxy for studying individual massive stars and quantifying their feedback contribution to the environment. We analyze eight exemplary targets in LMC N11 B from the Hubble UV Legacy Library of Young Stars as Essential Standards (ULLYSES) program using novel spectra from <i>HST<i/> (<i>COS<i/> and <i>STIS<i/>) in the UV, and from VLT (X-shooter) in the optical. We model the spectra of early to late O-type stars using state-of-the-art PoWR atmosphere models. We determine the stellar and wind parameters (e.g., <i>T<i/><sub>⋆<sub/>, log g, <i>L<i/><sub>⋆<sub/>, <i>Ṁ<i/>, and <i>v<i/><sub>∞<sub/>) of the analyzed objects, chemical abundances (C, N, and O), ionizing and mechanical feedback (<i>Q<i/><sub>H<sub/>, <i>Q<i/><sub>HeI<sub/>, <i>Q<i/><sub>He II<sub/>, and <i>L<i/><sub>mec<sub/>), and X-rays. We report ages of 2–4.5 Myr and masses of 30–60 M<sub>⊙<sub/> for the analyzed stars in N11 B, which are consistent with a scenario of sequential star formation. We note that the observed wind-momentum–luminosity relation is consistent with theoretical predictions. We detect nitrogen enrichment by up to a factor of seven in most of the stars. However, we do not find a correlation between nitrogen enrichment and projected rotational velocity. Finally, based on their spectral type, we estimate the total ionizing photons injected from the O-type stars in N11 B into its environment. We report log (Σ <i>Q<i/><sub>H<sub/>) = 50.5 ph s<sup>−1<sup/>, log (Σ <i>Q<i/><sub>He I<sub/>) = 49.6 ph s<sup>−1<sup/>, and log (Σ <i>Q<i/><sub>He II<sub/>)= 44.4 ph s<sup>−1<sup/>, consistent with the total ionizing budget in N11.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"20 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143665915","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-20DOI: 10.1051/0004-6361/202453455
M. Piecka, S. Hutschenreuter, J. Alves
The diffuse interstellar band (DIB) at 6196 Å exhibits notable profile variations across the Milky Way. This study addresses three open issues: the unusual broadening of the DIB profile towards Upper Sco, the lack of profile variations towards stars near η Car, and the origin of the blueshift observed in Sco OB1. Using archival spectra of 453 early-type stars across the Galactic disk and in its proximity, we created a catalogue of the DIB's profile parameters. Our analysis identified Doppler-split components within the DIB profiles across most regions with no evidence for these splits being able to account for the observed broadening (∼23 km s−1) in Upper Sco or other regions such as Orion, Vela OB2, and Melotte 20 (α Per cluster). We propose that neither the ages of the studied stellar populations nor the distances between clusters and nearby clouds significantly contribute to the broadening. However, we detect a gradient in the full width at half maximum within the Sco-Cen and Orion regions, where broadening decreases with distance from the star-forming centres. This result points to a possible connection between the DIB broadening and star formation (likely via the impact of recent supernovae). Regarding the Carina Nebula, we confirm the lack of DIB profile variations in a small region near η Car, although an adjacent southern area exhibits significant variations, comparable to those in Upper Sco. In addition to the Carina Nebula, we find that the Rosette Nebula and NGC 6405 also show consistently narrow profiles (< 20 km s−1) with minimal deviations from the median over spatial scales of a few parsecs. Finally, regarding the origin of the blueshift observed in Sco OB1, we used a comparison with the Lagoon Nebula and argue that the most natural explanation is the presence of an unresolved kinematic component in the profile of the DIB, shifting the measured centre of the band.
{"title":"Survey of profile parameters of the 6196 Å diffuse interstellar band","authors":"M. Piecka, S. Hutschenreuter, J. Alves","doi":"10.1051/0004-6361/202453455","DOIUrl":"https://doi.org/10.1051/0004-6361/202453455","url":null,"abstract":"The diffuse interstellar band (DIB) at 6196 Å exhibits notable profile variations across the Milky Way. This study addresses three open issues: the unusual broadening of the DIB profile towards Upper Sco, the lack of profile variations towards stars near <i>η<i/> Car, and the origin of the blueshift observed in Sco OB1. Using archival spectra of 453 early-type stars across the Galactic disk and in its proximity, we created a catalogue of the DIB's profile parameters. Our analysis identified Doppler-split components within the DIB profiles across most regions with no evidence for these splits being able to account for the observed broadening (∼23 km s<sup>−1<sup/>) in Upper Sco or other regions such as Orion, Vela OB2, and Melotte 20 (<i>α<i/> Per cluster). We propose that neither the ages of the studied stellar populations nor the distances between clusters and nearby clouds significantly contribute to the broadening. However, we detect a gradient in the full width at half maximum within the Sco-Cen and Orion regions, where broadening decreases with distance from the star-forming centres. This result points to a possible connection between the DIB broadening and star formation (likely via the impact of recent supernovae). Regarding the Carina Nebula, we confirm the lack of DIB profile variations in a small region near <i>η<i/> Car, although an adjacent southern area exhibits significant variations, comparable to those in Upper Sco. In addition to the Carina Nebula, we find that the Rosette Nebula and NGC 6405 also show consistently narrow profiles (< 20 km s<sup>−1<sup/>) with minimal deviations from the median over spatial scales of a few parsecs. Finally, regarding the origin of the blueshift observed in Sco OB1, we used a comparison with the Lagoon Nebula and argue that the most natural explanation is the presence of an unresolved kinematic component in the profile of the DIB, shifting the measured centre of the band.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"24 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143666022","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-03-20DOI: 10.1051/0004-6361/202453203
G. Di Gennaro, M. Brüggen, E. Moravec, L. Di Mascolo, R. J. van Weeren, G. Brunetti, R. Cassano, A. Botteon, E. Churazov, I. Khabibullin, N. Lyskova, F. de Gasperin, M. J. Hardcastle, H. J. A. Röttgering, T. Shimwell, R. Sunyaev, A. Stanford
Diffuse radio emission in galaxy clusters is a tracer of ultra-relativistic particles and μG-level magnetic fields, and is thought to be triggered by cluster merger events. In the distant Universe (i.e. z > 0.6), such sources have been observed only in a handful of systems, and their study is important to understand the evolution of large-scale magnetic fields over the cosmic time. Previous studies of nine Planck clusters up to z ∼ 0.9 suggest a fast amplification of cluster-scale magnetic fields, at least up to half of the current Universe’s age, and steep spectrum cluster scale emission, in line with particle re-acceleration due to turbulence. In this paper, we investigate the presence of diffuse radio emission in a larger sample of galaxy clusters reaching even higher redshifts (i.e. z ≳ 1). We selected clusters from the Massive and Distant Clusters of WISE Survey (MaDCoWS) with richness λ15 > 40 covering the area of the second data release of the LOFAR Two-Meter Sky Survey (LoTSS-DR2) at 144 MHz. These selected clusters are in the redshift range 0.78 − 1.53 (with a median value of 1.05). We detect the possible presence of diffuse radio emission, with the largest linear sizes of 350 − 500 kpc, in five out of the 56 clusters in our sample. If this diffuse radio emission is due to a radio halo, these radio sources lie on or above the scatter of the Pν − M500 radio halo correlations (at 150 MHz and 1.4 GHz) found at z < 0.6, depending on the mass assumed. We also find that these radio sources are at the limit of the detection by LoTSS, and therefore deeper observations are important for future studies.
{"title":"Limits and challenges of the detection of cluster-scale diffuse radio emission at high redshift","authors":"G. Di Gennaro, M. Brüggen, E. Moravec, L. Di Mascolo, R. J. van Weeren, G. Brunetti, R. Cassano, A. Botteon, E. Churazov, I. Khabibullin, N. Lyskova, F. de Gasperin, M. J. Hardcastle, H. J. A. Röttgering, T. Shimwell, R. Sunyaev, A. Stanford","doi":"10.1051/0004-6361/202453203","DOIUrl":"https://doi.org/10.1051/0004-6361/202453203","url":null,"abstract":"Diffuse radio emission in galaxy clusters is a tracer of ultra-relativistic particles and <i>μ<i/>G-level magnetic fields, and is thought to be triggered by cluster merger events. In the distant Universe (i.e. <i>z<i/> > 0.6), such sources have been observed only in a handful of systems, and their study is important to understand the evolution of large-scale magnetic fields over the cosmic time. Previous studies of nine <i>Planck<i/> clusters up to <i>z<i/> ∼ 0.9 suggest a fast amplification of cluster-scale magnetic fields, at least up to half of the current Universe’s age, and steep spectrum cluster scale emission, in line with particle re-acceleration due to turbulence. In this paper, we investigate the presence of diffuse radio emission in a larger sample of galaxy clusters reaching even higher redshifts (i.e. <i>z<i/> ≳ 1). We selected clusters from the Massive and Distant Clusters of <i>WISE<i/> Survey (MaDCoWS) with richness <i>λ<i/><sub>15<sub/> > 40 covering the area of the second data release of the LOFAR Two-Meter Sky Survey (LoTSS-DR2) at 144 MHz. These selected clusters are in the redshift range 0.78 − 1.53 (with a median value of 1.05). We detect the possible presence of diffuse radio emission, with the largest linear sizes of 350 − 500 kpc, in five out of the 56 clusters in our sample. If this diffuse radio emission is due to a radio halo, these radio sources lie on or above the scatter of the <i>P<i/><sub><i>ν<i/><sub/> − <i>M<i/><sub>500<sub/> radio halo correlations (at 150 MHz and 1.4 GHz) found at <i>z<i/> < 0.6, depending on the mass assumed. We also find that these radio sources are at the limit of the detection by LoTSS, and therefore deeper observations are important for future studies.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"93 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143666078","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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