Pub Date : 2025-03-21DOI: 10.1051/0004-6361/202453633
P. T. Rahna, M. Akhlaghi, C. López-Sanjuan, R. Logroño-García, D. J. Muniesa, H. Domínguez-Sánchez, J. A. Fernández-Ontiveros, D. Sobral, A. Lumbreras-Calle, A. L. Chies-Santos, J. E. Rodríguez-Martín, S. Eskandarlou, A. Ederoclite, A. Alvarez-Candal, H. Vázquez Ramió, A. J. Cenarro, A. Marín-Franch, J. Alcaniz, R. E. Angulo, D. Cristóbal-Hornillos, R. A. Dupke, C. Hernández-Monteagudo, M. Moles, L. Sodré, J. Varela
Aims. We present a dedicated automated pipeline to construct spatially resolved emission Hα+[NII] maps and to derive the spectral energy distributions (SEDs) in 12 optical filters (five broad and seven narrow and medium) of Hα emission line regions in nearby galaxies (z < 0.0165) observed by the Javalambre Photometric Local Universe Survey (J-PLUS).Methods. We used the J0660 filter of 140 Å width centered at 6600 Å to trace H α + [NII] emission, and r and i broad bands were used to estimate the stellar continuum. We created pure emission line images after the continnum subtraction, where the Hα emission line regions were detected. This method was also applied to integral field unit (IFU) spectroscopic data from PHANGS-MUSE, CALIFA, and MaNGA surveys by building synthetic narrow bands based on J-PLUS filters. The studied sample includes the cross-matched catalog of these IFU surveys with the J-PLUS third data release (DR3), amounting to two PHANGS-MUSE, 78 CALIFA, and 78 MaNGA galaxies at z < 0.0165, respectively.Results. We compared the Hα+[NII] radial profiles from J-PLUS and the IFU surveys, finding good agreement within the expected uncertainties. We also compared the SEDs from the emission line regions detected in J-PLUS images, reproducing the main spectral features present in the spectroscopic data. Finally, we compared the emission fluxes from the J-PLUS and IFU surveys accounting for scale differences, finding a difference of only 2% with a dispersion of 7% in the measurements.Conclusions. The J-PLUS data provide reliable spatially resolved Hα+[NII] emission maps for nearby galaxies. We provide the J-PLUS DR3 catalog for the 158 galaxies with IFU data, including emission maps, SEDs of star-forming clumps, and radial profiles.
{"title":"J-PLUS: Spectroscopic validation of Hα emission line maps in spatially resolved galaxies","authors":"P. T. Rahna, M. Akhlaghi, C. López-Sanjuan, R. Logroño-García, D. J. Muniesa, H. Domínguez-Sánchez, J. A. Fernández-Ontiveros, D. Sobral, A. Lumbreras-Calle, A. L. Chies-Santos, J. E. Rodríguez-Martín, S. Eskandarlou, A. Ederoclite, A. Alvarez-Candal, H. Vázquez Ramió, A. J. Cenarro, A. Marín-Franch, J. Alcaniz, R. E. Angulo, D. Cristóbal-Hornillos, R. A. Dupke, C. Hernández-Monteagudo, M. Moles, L. Sodré, J. Varela","doi":"10.1051/0004-6361/202453633","DOIUrl":"https://doi.org/10.1051/0004-6361/202453633","url":null,"abstract":"<i>Aims<i/>. We present a dedicated automated pipeline to construct spatially resolved emission H<i>α<i/>+[NII] maps and to derive the spectral energy distributions (SEDs) in 12 optical filters (five broad and seven narrow and medium) of H<i>α<i/> emission line regions in nearby galaxies (z < 0.0165) observed by the Javalambre Photometric Local Universe Survey (J-PLUS).<i>Methods<i/>. We used the <i>J<i/>0660 filter of 140 Å width centered at 6600 Å to trace H <i>α<i/> + [NII] emission, and <i>r<i/> and <i>i<i/> broad bands were used to estimate the stellar continuum. We created pure emission line images after the continnum subtraction, where the H<i>α<i/> emission line regions were detected. This method was also applied to integral field unit (IFU) spectroscopic data from PHANGS-MUSE, CALIFA, and MaNGA surveys by building synthetic narrow bands based on J-PLUS filters. The studied sample includes the cross-matched catalog of these IFU surveys with the J-PLUS third data release (DR3), amounting to two PHANGS-MUSE, 78 CALIFA, and 78 MaNGA galaxies at <i>z<i/> < 0.0165, respectively.<i>Results<i/>. We compared the H<i>α<i/>+[NII] radial profiles from J-PLUS and the IFU surveys, finding good agreement within the expected uncertainties. We also compared the SEDs from the emission line regions detected in J-PLUS images, reproducing the main spectral features present in the spectroscopic data. Finally, we compared the emission fluxes from the J-PLUS and IFU surveys accounting for scale differences, finding a difference of only 2% with a dispersion of 7% in the measurements.<i>Conclusions<i/>. The J-PLUS data provide reliable spatially resolved H<i>α<i/>+[NII] emission maps for nearby galaxies. We provide the J-PLUS DR3 catalog for the 158 galaxies with IFU data, including emission maps, SEDs of star-forming clumps, and radial profiles.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"59 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677466","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: 10.1051/0004-6361/202453196
J. A. López-Vázquez, M. Fernández-López, J. M. Girart, S. Curiel, R. Estalella, G. Busquet, L. A. Zapata, C.-F. Lee, R. Galván-Madrid
Context. Molecular outflows from massive protostars can impact the interstellar medium in different ways, adding turbulence on different spatial scales, dragging material at supersonic velocities, producing shocks and heating, and physically impinging onto dense structures that may be harboring other protostars.Aims. We aim to quantify the impact of the outflow associated with the high-mass protostar GGD 27-MM2(E) on its parent envelope and how this outflow affects its environment.Methods. We present Atacama Large Millimeter/submillimeter Array Band 3 observations of N2H+ (1–0) and CH3CN (5–4), as well as Band 7 observations of the H2CO molecular line emissions from the protostellar system GGD 27-MM2(E). Through position–velocity diagrams along and across the outflow axis, we studied the kinematics and structure of the outflow. We also fit extracted spectra of the CH3CN emission to obtain the physical conditions of the gas. We use the results to discuss the impact of the outflow on its surroundings.Results. We find that N2H+ emission traces a dense molecular cloud surrounding GGD 27-MM2(E). We estimate that the mass of this cloud is ~13.3–26.5 M⊙. The molecular cloud contains an internal cavity aligned with the H2CO-traced molecular outflow. The outflow, also traced by CH3CN, shows evidence of a collision with a molecular core (MC), as indicated by the distinctive increases in the distinct physical properties of the gas such as the excitation temperature, column density, line width, and velocity. This collision results in an X-shaped structure in the northern part of the outflow around the position of the MC, which produces spray-shocked material downstream in the north of MC, as observed in position–velocity diagrams both along and across the outflow axis. The outflow has a mass of 1.7–2.1 M⊙, a momentum of 7.8–10.1 M⊙ km s−1, a kinetic energy of 5.0–6.6×1044 erg, and a mass-loss rate of 4.9–6.0×10−4M⊙ yr−1.Conclusions. The molecular outflow from GGD 27-MM2(E) significantly perturbs and erodes its parent cloud, compressing the gas of sources such as the MC and ALMA 12. The feedback from this powerful protostellar outflow helps maintain the turbulence in the surrounding area.
{"title":"Erosion of a dense molecular core by a strong outflow from a massive protostar","authors":"J. A. López-Vázquez, M. Fernández-López, J. M. Girart, S. Curiel, R. Estalella, G. Busquet, L. A. Zapata, C.-F. Lee, R. Galván-Madrid","doi":"10.1051/0004-6361/202453196","DOIUrl":"https://doi.org/10.1051/0004-6361/202453196","url":null,"abstract":"<i>Context.<i/> Molecular outflows from massive protostars can impact the interstellar medium in different ways, adding turbulence on different spatial scales, dragging material at supersonic velocities, producing shocks and heating, and physically impinging onto dense structures that may be harboring other protostars.<i>Aims.<i/> We aim to quantify the impact of the outflow associated with the high-mass protostar GGD 27-MM2(E) on its parent envelope and how this outflow affects its environment.<i>Methods.<i/> We present Atacama Large Millimeter/submillimeter Array Band 3 observations of N<sub>2<sub/>H<sup>+<sup/> (1–0) and CH<sub>3<sub/>CN (5–4), as well as Band 7 observations of the H<sub>2<sub/>CO molecular line emissions from the protostellar system GGD 27-MM2(E). Through position–velocity diagrams along and across the outflow axis, we studied the kinematics and structure of the outflow. We also fit extracted spectra of the CH<sub>3<sub/>CN emission to obtain the physical conditions of the gas. We use the results to discuss the impact of the outflow on its surroundings.<i>Results.<i/> We find that N<sub>2<sub/>H<sup>+<sup/> emission traces a dense molecular cloud surrounding GGD 27-MM2(E). We estimate that the mass of this cloud is ~13.3–26.5 <i>M<i/><sub>⊙<sub/>. The molecular cloud contains an internal cavity aligned with the H<sub>2<sub/>CO-traced molecular outflow. The outflow, also traced by CH<sub>3<sub/>CN, shows evidence of a collision with a molecular core (MC), as indicated by the distinctive increases in the distinct physical properties of the gas such as the excitation temperature, column density, line width, and velocity. This collision results in an X-shaped structure in the northern part of the outflow around the position of the MC, which produces spray-shocked material downstream in the north of MC, as observed in position–velocity diagrams both along and across the outflow axis. The outflow has a mass of 1.7–2.1 <i>M<i/><sub>⊙<sub/>, a momentum of 7.8–10.1 <i>M<i/><sub>⊙<sub/> km s<sup>−1<sup/>, a kinetic energy of 5.0–6.6×10<sup>44<sup/> erg, and a mass-loss rate of 4.9–6.0×10<sup>−4<sup/> <i>M<i/><sub>⊙<sub/> yr<sup>−1<sup/>.<i>Conclusions.<i/> The molecular outflow from GGD 27-MM2(E) significantly perturbs and erodes its parent cloud, compressing the gas of sources such as the MC and ALMA 12. The feedback from this powerful protostellar outflow helps maintain the turbulence in the surrounding area.","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":"143677463","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: 10.1051/0004-6361/202453443
J. Varga, A. Matter, F. Millour, G. Weigelt, R. van Boekel, B. Lopez, F. Lykou, Á Kóspál, L. Chen, P. A. Boley, S. Wolf, M. Hogerheijde, A. Moór, P. Ábrahám, J.-C. Augereau, F. Cruz-Saenz de Miera, W.-C. Danchi, Th. Henning, T. Juhász, P. Priolet, M. Scheuck, J. Scigliuto, L. van Haastere, L. Zwicky
T CrA is a Herbig Ae-type young star in a complex circumstellar environment; it includes a circumstellar disk, accretion streamers, jets, and outflows. It has long been suspected to be a binary. However, until now, there has been no direct detection of a companion. Here we present new VLTI/MATISSE L- and N-band observations of T CrA taken between 2023 May and 2024 August with the aim of testing the binary nature of the system. We modeled the data with a geometric model using the Python tool oimodeler. We detected a companion (T CrA B) with a projected separation of Δr = 153.2 ± 1.2 mas (≈23 au) toward the west direction at a position angle of 275.4 ± 0.1°, in 2024 May–August. Our results support that the companion has a nearly edge-on orbit that is highly misaligned with respect to the circumprimary disk. Such a configuration could cause warping and tearing of the disk around the primary, which has been proposed by recent studies. In the L band the companion is extended, with a full width at half maximum (FWHM) size of ∼1 au, suggesting that the emission comes from a disk around the secondary star. The companion flux is 0.2–0.3 Jy in the L band, and 0.2–0.7 Jy in the N band, accounting for 4–20% of the total emission at those wavelengths. The SED of the companion is compatible with thermal radiation of warm dust (600–800 K).
{"title":"T CrA has a companion","authors":"J. Varga, A. Matter, F. Millour, G. Weigelt, R. van Boekel, B. Lopez, F. Lykou, Á Kóspál, L. Chen, P. A. Boley, S. Wolf, M. Hogerheijde, A. Moór, P. Ábrahám, J.-C. Augereau, F. Cruz-Saenz de Miera, W.-C. Danchi, Th. Henning, T. Juhász, P. Priolet, M. Scheuck, J. Scigliuto, L. van Haastere, L. Zwicky","doi":"10.1051/0004-6361/202453443","DOIUrl":"https://doi.org/10.1051/0004-6361/202453443","url":null,"abstract":"T CrA is a Herbig Ae-type young star in a complex circumstellar environment; it includes a circumstellar disk, accretion streamers, jets, and outflows. It has long been suspected to be a binary. However, until now, there has been no direct detection of a companion. Here we present new VLTI/MATISSE <i>L<i/>- and <i>N<i/>-band observations of T CrA taken between 2023 May and 2024 August with the aim of testing the binary nature of the system. We modeled the data with a geometric model using the Python tool oimodeler. We detected a companion (T CrA B) with a projected separation of Δ<i>r<i/> = 153.2 ± 1.2 mas (≈23 au) toward the west direction at a position angle of 275.4 ± 0.1°, in 2024 May–August. Our results support that the companion has a nearly edge-on orbit that is highly misaligned with respect to the circumprimary disk. Such a configuration could cause warping and tearing of the disk around the primary, which has been proposed by recent studies. In the <i>L<i/> band the companion is extended, with a full width at half maximum (FWHM) size of ∼1 au, suggesting that the emission comes from a disk around the secondary star. The companion flux is 0.2–0.3 Jy in the <i>L<i/> band, and 0.2–0.7 Jy in the <i>N<i/> band, accounting for 4–20% of the total emission at those wavelengths. The SED of the companion is compatible with thermal radiation of warm dust (600–800 K).","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"12 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677770","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: 10.1051/0004-6361/202453359
Lionel Mulato, Jaroslav Merc, Stéphane Charbonnel, Olivier Garde, Pascal Le Dȗ, Thomas Petit
Context. Gaia DR3, released in June 2022, included low-resolution XP spectra that have been used for the classification of various types of emission-line objects through machine-learning techniques. The Gaia Extended Stellar Parametrizer for Emission-Line Stars (ESP-ELS) algorithm identified 565 sources as potential Wolf-Rayet (WR) stars. Over half of them were already known as WR stars in the Milky Way and Magellanic Clouds.Aims. We utilized Gaia DR3 data to identify new Galactic WR stars.Methods. We extracted all sources from the Gaia catalog classified as WC- or WN-type stars by the ESP-ELS algorithm. By applying judicious 2MASS color selection criteria, leveraging Gaia Hα measurements, and filtering out objects already cataloged in various databases, we selected 37 bright candidates (G ≤ 16 mag) and 22 faint candidates (G > 16 mag). Spectroscopic follow-up observations of these candidates were conducted using the 2SPOT facilities in Chile and France, as well as the 1 m C2PU’s Epsilon telescope at the Calern Observatory.Results. This paper focuses on the brighter sample. Among the 37 targets, we confirmed 17 and 16 new Galactic WC- and WN-type WR stars, respectively. Three of them were recently reported as new WR stars in an independent study.Conclusions. The Gaia mission provides a valuable resource for identifying WR stars missed in earlier surveys. While this work concentrated on a relatively small starting sample provided by the ESP-ELS algorithm, our findings highlight the potential for refining selection criteria to identify additional candidates not included in the outputs of the algorithm. Furthermore, the observation program underscores the utility of small telescopes in acquiring initial spectral data for sources with magnitudes up to G ~ 16 mag.
{"title":"Search for new Galactic Wolf–Rayet stars using Gaia DR3","authors":"Lionel Mulato, Jaroslav Merc, Stéphane Charbonnel, Olivier Garde, Pascal Le Dȗ, Thomas Petit","doi":"10.1051/0004-6361/202453359","DOIUrl":"https://doi.org/10.1051/0004-6361/202453359","url":null,"abstract":"<i>Context. Gaia<i/> DR3, released in June 2022, included low-resolution XP spectra that have been used for the classification of various types of emission-line objects through machine-learning techniques. The <i>Gaia Extended Stellar Parametrizer for Emission-Line Stars<i/> (ESP-ELS) algorithm identified 565 sources as potential Wolf-Rayet (WR) stars. Over half of them were already known as WR stars in the Milky Way and Magellanic Clouds.<i>Aims.<i/> We utilized <i>Gaia<i/> DR3 data to identify new Galactic WR stars.<i>Methods.<i/> We extracted all sources from the <i>Gaia<i/> catalog classified as WC- or WN-type stars by the ESP-ELS algorithm. By applying judicious 2MASS color selection criteria, leveraging <i>Gaia<i/> H<i>α<i/> measurements, and filtering out objects already cataloged in various databases, we selected 37 bright candidates (<i>G<i/> ≤ 16 mag) and 22 faint candidates (<i>G ><i/> 16 mag). Spectroscopic follow-up observations of these candidates were conducted using the 2SPOT facilities in Chile and France, as well as the 1 m C2PU’s Epsilon telescope at the Calern Observatory.<i>Results.<i/> This paper focuses on the brighter sample. Among the 37 targets, we confirmed 17 and 16 new Galactic WC- and WN-type WR stars, respectively. Three of them were recently reported as new WR stars in an independent study.<i>Conclusions.<i/> The <i>Gaia<i/> mission provides a valuable resource for identifying WR stars missed in earlier surveys. While this work concentrated on a relatively small starting sample provided by the ESP-ELS algorithm, our findings highlight the potential for refining selection criteria to identify additional candidates not included in the outputs of the algorithm. Furthermore, the observation program underscores the utility of small telescopes in acquiring initial spectral data for sources with magnitudes up to <i>G ~<i/> 16 mag.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"35 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677460","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: 10.1051/0004-6361/202453352
M. Vivek, Dominika Wylezalek
Context. Broad absorption line (BAL) quasars exhibit significant outflows, offering insights into active galactic nucleus (AGN) feedback. While typically associated with high Eddington ratios, BAL quasars also occur in low Eddington ratio regimes, which remain poorly understood. The aim of this study is to compare BAL properties and variability across these regimes.Aims. We investigate the occurrence rates, absorption characteristics, and variability of BAL quasars at low and high Eddington ratios.Methods. Using the SDSS DR16 quasar catalog, we selected a redshift-matched control sample to compare low and high Eddington ratio BAL quasar sources. We first examined the BAL fraction as a function of Eddington ratio. Key absorption parameters (equivalent width, absorption line width, velocity range, and depth) were analyzed, and a multi-epoch variability study was conducted using repeat spectra, followed by a comparison of parameter distributions between the two samples.Results. For the first time, we report an increase in the BAL fraction toward low Eddington ratios, in addition to the previously known trend of high BAL fraction at high Eddington ratios. While high Eddington sources show extreme absorption features, overall distributions are statistically similar except for maximum outflow velocity. No significant variability differences were observed. The correlation between outflow velocity, Eddington ratio, and luminosity supports the role of radiation pressure in driving quasar outflows. For low Eddington ratios, additional mechanisms, such as softer SEDs, larger outflow distances, and thickened accretion disks from radiatively inefficient processes, likely drive outflow formation.
{"title":"Broad absorption line outflows are common in low Eddington ratio active galactic nuclei","authors":"M. Vivek, Dominika Wylezalek","doi":"10.1051/0004-6361/202453352","DOIUrl":"https://doi.org/10.1051/0004-6361/202453352","url":null,"abstract":"<i>Context.<i/> Broad absorption line (BAL) quasars exhibit significant outflows, offering insights into active galactic nucleus (AGN) feedback. While typically associated with high Eddington ratios, BAL quasars also occur in low Eddington ratio regimes, which remain poorly understood. The aim of this study is to compare BAL properties and variability across these regimes.<i>Aims.<i/> We investigate the occurrence rates, absorption characteristics, and variability of BAL quasars at low and high Eddington ratios.<i>Methods.<i/> Using the SDSS DR16 quasar catalog, we selected a redshift-matched control sample to compare low and high Eddington ratio BAL quasar sources. We first examined the BAL fraction as a function of Eddington ratio. Key absorption parameters (equivalent width, absorption line width, velocity range, and depth) were analyzed, and a multi-epoch variability study was conducted using repeat spectra, followed by a comparison of parameter distributions between the two samples.<i>Results.<i/> For the first time, we report an increase in the BAL fraction toward low Eddington ratios, in addition to the previously known trend of high BAL fraction at high Eddington ratios. While high Eddington sources show extreme absorption features, overall distributions are statistically similar except for maximum outflow velocity. No significant variability differences were observed. The correlation between outflow velocity, Eddington ratio, and luminosity supports the role of radiation pressure in driving quasar outflows. For low Eddington ratios, additional mechanisms, such as softer SEDs, larger outflow distances, and thickened accretion disks from radiatively inefficient processes, likely drive outflow formation.","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":"143677764","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: 10.1051/0004-6361/202451340
J. Necker, E. Graikou, M. Kowalski, A. Franckowiak, J. Nordin, T. Pernice, S. van Velzen, P. M. Veres
Context. Observations of transient emission from extreme accretion events onto supermassive black holes can reveal conditions in the center of galaxies and the black hole itself. Most recently, it has been suggested these sources could be emitters of high-energy neutrinos. However, in most cases, it remains unclear whether this would be classified as the outcome of rejuvenated accretion or a tidal disruption event (TDE).Aims. We expand on existing samples of infrared (IR) flares to compile the largest and most complete list available. A large sample size is necessary to provide high-enough statistics for distant and faint objects to estimate their rates. Our catalog is large enough to facilitate a preliminary study of the rate evolution with redshift for the first time.Methods. We compiled a sample of 40 million galaxies. Using a custom, publicly available pipeline, we analyzed the WISE light curves for these 40 million objects using the Bayesian Blocks algorithm. We selected promising for dust echo candidates involved in transient accretion events and we inferred the luminosity, extension, and temperature of the hot dust by fitting a blackbody spectrum.Results. We established a clean sample of 823 dust echo-like IR flares, dubbed the Flaires catalog. For 568 of them, we were able to estimate the dust properties. After removing 70 objects with possible contributions from synchrotron emission, the luminosity, extension, and temperature are consistent with dust echos. Estimating the dust extension from the light curve shape revealed that the duration of the incident flare is broadly compatible with the duration of TDEs. The resulting rate per galaxy is consistent with the latest measurements of IR-detected TDEs and appears to decline with increasing redshift.Conclusions. Although systematic uncertainties may impact the calculation of the rate evolution, this catalog will enable further research of phenomena related to dust echos from TDEs and extreme accretion flares.
{"title":"Flaires","authors":"J. Necker, E. Graikou, M. Kowalski, A. Franckowiak, J. Nordin, T. Pernice, S. van Velzen, P. M. Veres","doi":"10.1051/0004-6361/202451340","DOIUrl":"https://doi.org/10.1051/0004-6361/202451340","url":null,"abstract":"<i>Context.<i/> Observations of transient emission from extreme accretion events onto supermassive black holes can reveal conditions in the center of galaxies and the black hole itself. Most recently, it has been suggested these sources could be emitters of high-energy neutrinos. However, in most cases, it remains unclear whether this would be classified as the outcome of rejuvenated accretion or a tidal disruption event (TDE).<i>Aims.<i/> We expand on existing samples of infrared (IR) flares to compile the largest and most complete list available. A large sample size is necessary to provide high-enough statistics for distant and faint objects to estimate their rates. Our catalog is large enough to facilitate a preliminary study of the rate evolution with redshift for the first time.<i>Methods.<i/> We compiled a sample of 40 million galaxies. Using a custom, publicly available pipeline, we analyzed the WISE light curves for these 40 million objects using the Bayesian Blocks algorithm. We selected promising for dust echo candidates involved in transient accretion events and we inferred the luminosity, extension, and temperature of the hot dust by fitting a blackbody spectrum.<i>Results.<i/> We established a clean sample of 823 dust echo-like IR flares, dubbed the Flaires catalog. For 568 of them, we were able to estimate the dust properties. After removing 70 objects with possible contributions from synchrotron emission, the luminosity, extension, and temperature are consistent with dust echos. Estimating the dust extension from the light curve shape revealed that the duration of the incident flare is broadly compatible with the duration of TDEs. The resulting rate per galaxy is consistent with the latest measurements of IR-detected TDEs and appears to decline with increasing redshift.<i>Conclusions.<i/> Although systematic uncertainties may impact the calculation of the rate evolution, this catalog will enable further research of phenomena related to dust echos from TDEs and extreme accretion flares.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"28 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677771","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: 10.1051/0004-6361/202453227
C. O. Obasi, E. R. Garro, J. G. Fernández-Trincado, D. Minniti, M. Gómez, M. C. Parisi, M. Ortigoza-Urdaneta
Context. With the rise of large surveys across wavelengths, both supervised and unsupervised machine learning algorithms have increasingly aided in detecting large samples of old open clusters in high-extinction regions of the Milky Way bulge and disk.Aims. Our primary goal is to confirm or discard automatically detected open clusters from poorly studied, heavily contaminated regions of the Milky Way. Cleaning these samples is critical for reconstructing the Galactic disk’s star formation history and understanding the thin and thick disk formation model.Methods. We used data from the VVVX, 2MASS, and Gaia DR3 surveys to confirm and characterize nine open cluster candidates: BH118, BH 144, Schuster-MWSC 1756, Saurer 3, FSR 1521, Saurer 2, Haffner 10-FSR 1231, Juchert 12, and Pismis 3. We constructed density maps and vector–proper motion diagrams to analyse the targets and performed photometric analysis to derive their main physical parameters.Results. We examined cluster images from the 2MASS, WISE, and DECaPS surveys, identifying star clusters through an over-density of stars. This was confirmed with a VVVX photometry density map and validated using Gaussian kernel density estimation. Using Gaia proper motion data, we refined cluster memberships and decontaminated the data to build the final cluster catalogue with objects with a high probability of being star cluster members. We derived the following parameters: extinction values (AKs) ranging from 0.07±0.03 to 0.50±0.04; colour excess values (E(J-Ks)) from 0.16±0.03 to 0.60±0.03; distances (D) from 2.19±0.06 kpc to 8.94±0.06 kpc; Galactocentric distances (RG) from 7.82 kpc to 15.08 kpc; vertical distance component values (Z) from −0.09 kpc to 0.34 kpc; and tangential velocities (VT) from 30.59 km/s to 245.42 km/s. We also computed ages and metallicities by fitting PARSEC isochrones, finding ages (t) ranging from 20 Myr to 5 Gyr and metallicities ([Fe/H]) from −0.5 to 0.5. Structural parameters include core radii (rc) from 0.71′ to 5.21′, tidal radii (rt) from 3.4′ to 12.0′, and concentration indices (c) from 0.36 to 0.83.Conclusions. We photometrically confirm the open cluster nature for the nine targets in our compilation and updated their main physical parameters.
{"title":"Multi-wavelength characterization of VVVX open clusters","authors":"C. O. Obasi, E. R. Garro, J. G. Fernández-Trincado, D. Minniti, M. Gómez, M. C. Parisi, M. Ortigoza-Urdaneta","doi":"10.1051/0004-6361/202453227","DOIUrl":"https://doi.org/10.1051/0004-6361/202453227","url":null,"abstract":"<i>Context.<i/> With the rise of large surveys across wavelengths, both supervised and unsupervised machine learning algorithms have increasingly aided in detecting large samples of old open clusters in high-extinction regions of the Milky Way bulge and disk.<i>Aims.<i/> Our primary goal is to confirm or discard automatically detected open clusters from poorly studied, heavily contaminated regions of the Milky Way. Cleaning these samples is critical for reconstructing the Galactic disk’s star formation history and understanding the thin and thick disk formation model.<i>Methods.<i/> We used data from the VVVX, 2MASS, and <i>Gaia<i/> DR3 surveys to confirm and characterize nine open cluster candidates: BH118, BH 144, Schuster-MWSC 1756, Saurer 3, FSR 1521, Saurer 2, Haffner 10-FSR 1231, Juchert 12, and Pismis 3. We constructed density maps and vector–proper motion diagrams to analyse the targets and performed photometric analysis to derive their main physical parameters.<i>Results.<i/> We examined cluster images from the 2MASS, WISE, and DECaPS surveys, identifying star clusters through an over-density of stars. This was confirmed with a VVVX photometry density map and validated using Gaussian kernel density estimation. Using <i>Gaia<i/> proper motion data, we refined cluster memberships and decontaminated the data to build the final cluster catalogue with objects with a high probability of being star cluster members. We derived the following parameters: extinction values (A<sub><i>Ks<i/><sub/>) ranging from 0.07±0.03 to 0.50±0.04; colour excess values (E(J-K<sub><i>s<i/><sub/>)) from 0.16±0.03 to 0.60±0.03; distances (D) from 2.19±0.06 kpc to 8.94±0.06 kpc; Galactocentric distances (R<sub><i>G<i/><sub/>) from 7.82 kpc to 15.08 kpc; vertical distance component values (Z) from −0.09 kpc to 0.34 kpc; and tangential velocities (V<sub><i>T<i/><sub/>) from 30.59 km/s to 245.42 km/s. We also computed ages and metallicities by fitting PARSEC isochrones, finding ages (t) ranging from 20 Myr to 5 Gyr and metallicities ([Fe/H]) from −0.5 to 0.5. Structural parameters include core radii (r<sub><i>c<i/><sub/>) from 0.71′ to 5.21′, tidal radii (r<sub><i>t<i/><sub/>) from 3.4′ to 12.0′, and concentration indices (c) from 0.36 to 0.83.<i>Conclusions.<i/> We photometrically confirm the open cluster nature for the nine targets in our compilation and updated their main physical parameters.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"46 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677533","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: 10.1051/0004-6361/202553692
K. Deshmukh, T. Shenar, A. Mérand, H. Sana, P. Marchant, G. A. Wade, J. Bodensteiner, A.-N. Chené, A. J. Frost, A. Gilkis, N. Langer, L. Oskinova
HD 45166 was recently reported to be a long-period binary comprising a B7 V star and a highly magnetic (⟨B⟩=43.0 ± 0.5 kG) hot Wolf-Rayet-like component, dubbed a quasi Wolf-Rayet (qWR) star in the literature. While originally proposed to be a short-period binary, long-term spectroscopic monitoring suggested a 22.5 yr orbital period. With a derived dynamical mass of 2.03 ± 0.44 M⊙, the qWR component is the most strongly magnetized non-degenerate object ever detected and a potential magnetar progenitor. However, the long period renders the spectroscopic orbital solution and dynamical mass estimates uncertain, casting doubts on whether the qWR component is massive enough to undergo core collapse. Here, we spatially resolve the HD 45166 binary using newly acquired interferometric data obtained with the GRAVITY instrument of the Very Large Telescope Interferometer. Due to the calibrator star being a binary as well, we implemented a new approach for visibility calibration and tested it thoroughly using archival GRAVITY data. The newly calibrated HD 45166 data revealed the unmistakable presence of a companion to the qWR component with an angular separation of 10.9 ± 0.1 mas (which translates to a projected physical separation of 10.8 ± 0.4 au), consistent with the long-period orbit. We obtained a model-independent qWR mass using interferometric and spectroscopic data together. This observation robustly confirms that HD 45166 is truly a long-period binary and provides an anchor point for accurate mass determination of the qWR component with further observations.
{"title":"The highly magnetic Wolf-Rayet binary HD 45166 resolved with VLTI/GRAVITY⋆","authors":"K. Deshmukh, T. Shenar, A. Mérand, H. Sana, P. Marchant, G. A. Wade, J. Bodensteiner, A.-N. Chené, A. J. Frost, A. Gilkis, N. Langer, L. Oskinova","doi":"10.1051/0004-6361/202553692","DOIUrl":"https://doi.org/10.1051/0004-6361/202553692","url":null,"abstract":"HD 45166 was recently reported to be a long-period binary comprising a B7 V star and a highly magnetic (⟨<i>B<i/>⟩=43.0 ± 0.5 kG) hot Wolf-Rayet-like component, dubbed a quasi Wolf-Rayet (qWR) star in the literature. While originally proposed to be a short-period binary, long-term spectroscopic monitoring suggested a 22.5 yr orbital period. With a derived dynamical mass of 2.03 ± 0.44 <i>M<i/><sub>⊙<sub/>, the qWR component is the most strongly magnetized non-degenerate object ever detected and a potential magnetar progenitor. However, the long period renders the spectroscopic orbital solution and dynamical mass estimates uncertain, casting doubts on whether the qWR component is massive enough to undergo core collapse. Here, we spatially resolve the HD 45166 binary using newly acquired interferometric data obtained with the GRAVITY instrument of the Very Large Telescope Interferometer. Due to the calibrator star being a binary as well, we implemented a new approach for visibility calibration and tested it thoroughly using archival GRAVITY data. The newly calibrated HD 45166 data revealed the unmistakable presence of a companion to the qWR component with an angular separation of 10.9 ± 0.1 mas (which translates to a projected physical separation of 10.8 ± 0.4 au), consistent with the long-period orbit. We obtained a model-independent qWR mass using interferometric and spectroscopic data together. This observation robustly confirms that HD 45166 is truly a long-period binary and provides an anchor point for accurate mass determination of the qWR component with further observations.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"18 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677769","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: 10.1051/0004-6361/202453169
A. Ippolito, B. Sánchez-Cano, Y. Harada
Context. During September 2014, intense solar activity led to a number of coronal mass ejections (CMEs) propagating in the heliosphere. The strong perturbation in the interplanetary magnetic field and the remarkable enhancements in the energetic particle fluxes accelerated by the shock waves associated with the CMEs affected the environments of the inner planets of the Solar System.Aims. Taking advantage of a relatively favorable position in terms of angular distance among Mercury, Earth, and Mars, our purpose is to observe the evolution and impact of strong solar events, providing an overview of the impact of the same solar phenomena on different planetary environments, with special interest in the response of Mars’ ionosphere as this may have implications for future exploration of the red planet.Methods. We used observations from a fleet of spacecraft distributed in the inner Solar System, such as STEREO B, MESSENGER, Mars Express, and SOHO, to perform a characterization of the interaction with the planets, investigating some of the main effects of the CMEs on the different planetary environments. Besides, we applied a numerical simulation to reconstruct the magnetic connection from Mercury, Earth, and Mars to the solar corona on the dates on which the CME events occurred.Results. We find that the CMEs events analyzed here induced remarkable effects that affected all the environments of the inner planets of the Solar System. Enhancements in the solar energetic particle fluxes were observed at Mercury, Earth, and Mars, with different characteristics. In addition, a solar radio burst was observed both at Earth and Mars, together with strong disturbances in the geomagnetic field, and diffuse echoes and radio black outs in the Martian ionosphere.Conclusions. The proposed multi-spacecraft and multiparameter analysis, along with the numerical simulations for reconstructing the magnetic footpoints of the Parker spiral on the Sun’s surface, offer a detailed cause-and-effect framework for studying space weather events in the Solar System.
{"title":"Effects of the September 2014 coronal mass ejection chain in the inner Solar System and the response of the Martian ionosphere","authors":"A. Ippolito, B. Sánchez-Cano, Y. Harada","doi":"10.1051/0004-6361/202453169","DOIUrl":"https://doi.org/10.1051/0004-6361/202453169","url":null,"abstract":"<i>Context.<i/> During September 2014, intense solar activity led to a number of coronal mass ejections (CMEs) propagating in the heliosphere. The strong perturbation in the interplanetary magnetic field and the remarkable enhancements in the energetic particle fluxes accelerated by the shock waves associated with the CMEs affected the environments of the inner planets of the Solar System.<i>Aims.<i/> Taking advantage of a relatively favorable position in terms of angular distance among Mercury, Earth, and Mars, our purpose is to observe the evolution and impact of strong solar events, providing an overview of the impact of the same solar phenomena on different planetary environments, with special interest in the response of Mars’ ionosphere as this may have implications for future exploration of the red planet.<i>Methods.<i/> We used observations from a fleet of spacecraft distributed in the inner Solar System, such as STEREO B, MESSENGER, Mars Express, and SOHO, to perform a characterization of the interaction with the planets, investigating some of the main effects of the CMEs on the different planetary environments. Besides, we applied a numerical simulation to reconstruct the magnetic connection from Mercury, Earth, and Mars to the solar corona on the dates on which the CME events occurred.<i>Results.<i/> We find that the CMEs events analyzed here induced remarkable effects that affected all the environments of the inner planets of the Solar System. Enhancements in the solar energetic particle fluxes were observed at Mercury, Earth, and Mars, with different characteristics. In addition, a solar radio burst was observed both at Earth and Mars, together with strong disturbances in the geomagnetic field, and diffuse echoes and radio black outs in the Martian ionosphere.<i>Conclusions.<i/> The proposed multi-spacecraft and multiparameter analysis, along with the numerical simulations for reconstructing the magnetic footpoints of the Parker spiral on the Sun’s surface, offer a detailed cause-and-effect framework for studying space weather events in the Solar System.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"71 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677467","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: 10.1051/0004-6361/202453324
J. Haas, P. Kroupa, L. Šubr, M. Singhal
Context. Various past theoretical considerations and observational efforts suggest the presence of a population of stellar-mass black holes in the innermost parsec of the Galactic centre.Aims. In this Letter, we investigate the impact of these black holes on the composition of the embedding stellar population through their direct collisions with the individual stars. Based on the estimated collision rates, we derive an order of magnitude radial density profile of the black hole cluster.Methods. The estimates were obtained analytically, considering various possible formation channels for the black holes and the observed present-day properties of the stellar populations in the Galactic centre.Results. We find that the collisions of the stars and the black holes can lead to the depletion of the most massive stars within the S-cluster on a timescale of a few million years. The necessary black hole cluster density is compatible with the recurrent in situ star formation in the innermost parsec of the Galactic centre. We suggest that such a depletion naturally explains the reported lack of stars of the stellar type O and of the Galactic halo hyper-velocity star counterparts within the S-cluster.
{"title":"The star grinder in the Galactic centre","authors":"J. Haas, P. Kroupa, L. Šubr, M. Singhal","doi":"10.1051/0004-6361/202453324","DOIUrl":"https://doi.org/10.1051/0004-6361/202453324","url":null,"abstract":"<i>Context.<i/> Various past theoretical considerations and observational efforts suggest the presence of a population of stellar-mass black holes in the innermost parsec of the Galactic centre.<i>Aims.<i/> In this Letter, we investigate the impact of these black holes on the composition of the embedding stellar population through their direct collisions with the individual stars. Based on the estimated collision rates, we derive an order of magnitude radial density profile of the black hole cluster.<i>Methods.<i/> The estimates were obtained analytically, considering various possible formation channels for the black holes and the observed present-day properties of the stellar populations in the Galactic centre.<i>Results.<i/> We find that the collisions of the stars and the black holes can lead to the depletion of the most massive stars within the S-cluster on a timescale of a few million years. The necessary black hole cluster density is compatible with the recurrent in situ star formation in the innermost parsec of the Galactic centre. We suggest that such a depletion naturally explains the reported lack of stars of the stellar type O and of the Galactic halo hyper-velocity star counterparts within the S-cluster.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"35 1","pages":""},"PeriodicalIF":6.5,"publicationDate":"2025-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143677591","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}
京公网安备 11010802042870号
京ICP备2023020795号-1
扫码关注我们
求助内容：
应助结果提醒方式：