Pub Date : 2024-06-12DOI: 10.1051/0004-6361/202347999
Jyoti Yadav, Vikrant V. Jadhav
Galaxy interactions in groups can lead to intense starburst and activation of active galactic nuclei (AGN). The stripped gas from the outer disk can lead to star-forming clumps along the tidal tails or sometimes tidal dwarf galaxies. We investigate the impact of interaction on various galaxy properties, including morphology, star formation rates, and chemical composition in the galaxy group AM,1054-325 using Multi Unit Spectroscopic Explorer (MUSE) data. We conduct a comprehensive spatially and spectrally resolved investigation of star formation rate, star formation histories, metallicity and AGN activity. The galaxy subgroup AM,1054-325A shows multiple star-forming clumps in Halpha emission along the western tidal tail, which are formed due to the tidal stripping. These clumps also have higher metallicity. AM,1054-325B is quenched and shows disturbed gas kinematics and the signature of gas accretion in the Halpha map. The specific star formation along the tidal tail is higher, contributing to the galaxy's overall stellar mass growth.
{"title":"The morphology and kinematics of the galaxy group AM1054-325: A MUSE perspective","authors":"Jyoti Yadav, Vikrant V. Jadhav","doi":"10.1051/0004-6361/202347999","DOIUrl":"https://doi.org/10.1051/0004-6361/202347999","url":null,"abstract":"Galaxy interactions in groups can lead to intense starburst and activation of active galactic nuclei (AGN). The stripped gas from the outer disk can lead to star-forming clumps along the tidal tails or sometimes tidal dwarf galaxies. We investigate the impact of interaction on various galaxy properties, including morphology, star formation rates, and chemical composition in the galaxy group AM,1054-325 using Multi Unit Spectroscopic Explorer (MUSE) data. We conduct a comprehensive spatially and spectrally resolved investigation of star formation rate, star formation histories, metallicity and AGN activity. The galaxy subgroup AM,1054-325A shows multiple star-forming clumps in Halpha emission along the western tidal tail, which are formed due to the tidal stripping. These clumps also have higher metallicity. AM,1054-325B is quenched and shows disturbed gas kinematics and the signature of gas accretion in the Halpha map. The specific star formation along the tidal tail is higher, contributing to the galaxy's overall stellar mass growth.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":"33 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141353653","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-12DOI: 10.1051/0004-6361/202449549
P. Galli, N. Miret-Roig, H. Bouy, J. Olivares, D. Barrado
Octans is one of the most distant ($d pc) young stellar associations of the solar neighbourhood, and it has not yet been sufficiently explored. Its age is still poorly constrained in the literature and requires further investigation. We take advantage of the state-of-the-art astrometry delivered by the third data release of the Gaia space mission combined with radial velocity measurements obtained from high-resolution spectroscopy to compute the 3D positions and 3D spatial velocities of the stars and derive the dynamical traceback age of the association. We created a clean sample of cluster members by removing potential outliers from our initial list of candidate members. We then performed an extensive traceback analysis using different subsamples of stars, different metrics to define the size of the association, and different models for the Galactic potential to integrate the stellar orbits in the past. We derive a dynamical age of $34^ $ Myr that is independent from stellar models and represents the most precise age estimate currently available for the Octans association. After correcting the radial velocity of the stars for the effect of gravitational redshift, we obtain a dynamical age of $33^ $ Myr, which is in very good agreement with our first solution. This shows that the effect of gravitational redshift is small for such a distant young stellar association. Our result is also consistent with the less accurate age estimates obtained in previous studies from lithium depletion (30-40 Myr) and isochrones (20-30 Myr). By integrating the stellar orbits in time, we show that the members of Octans and Octans-Near had different locations in the past, which indicates that the two associations are unrelated despite the close proximity in the sky. This is the first reliable and precise dynamical age result for the Octans young stellar association. Our results confirm that it is possible to derive precise dynamical ages via the traceback method for $ Myr old stellar clusters at about $ pc with the same precision level that has been achieved in other studies for young stellar groups within 50 pc of the Sun. This represents one more step towards constructing a self-consistent age scale based on the 3D space motion of the stars in the young stellar clusters of the solar neighbourhood.
{"title":"Dynamical traceback age of the Octans young stellar association","authors":"P. Galli, N. Miret-Roig, H. Bouy, J. Olivares, D. Barrado","doi":"10.1051/0004-6361/202449549","DOIUrl":"https://doi.org/10.1051/0004-6361/202449549","url":null,"abstract":"Octans is one of the most distant ($d pc) young stellar associations of the solar neighbourhood, and it has not yet been sufficiently explored. Its age is still poorly constrained in the literature and requires further investigation. We take advantage of the state-of-the-art astrometry delivered by the third data release of the Gaia space mission combined with radial velocity measurements obtained from high-resolution spectroscopy to compute the 3D positions and 3D spatial velocities of the stars and derive the dynamical traceback age of the association. We created a clean sample of cluster members by removing potential outliers from our initial list of candidate members. We then performed an extensive traceback analysis using different subsamples of stars, different metrics to define the size of the association, and different models for the Galactic potential to integrate the stellar orbits in the past. We derive a dynamical age of $34^ $ Myr that is independent from stellar models and represents the most precise age estimate currently available for the Octans association. After correcting the radial velocity of the stars for the effect of gravitational redshift, we obtain a dynamical age of $33^ $ Myr, which is in very good agreement with our first solution. This shows that the effect of gravitational redshift is small for such a distant young stellar association. Our result is also consistent with the less accurate age estimates obtained in previous studies from lithium depletion (30-40 Myr) and isochrones (20-30 Myr). By integrating the stellar orbits in time, we show that the members of Octans and Octans-Near had different locations in the past, which indicates that the two associations are unrelated despite the close proximity in the sky. This is the first reliable and precise dynamical age result for the Octans young stellar association. Our results confirm that it is possible to derive precise dynamical ages via the traceback method for $ Myr old stellar clusters at about $ pc with the same precision level that has been achieved in other studies for young stellar groups within 50 pc of the Sun. This represents one more step towards constructing a self-consistent age scale based on the 3D space motion of the stars in the young stellar clusters of the solar neighbourhood.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":"34 41","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141354263","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-12DOI: 10.1051/0004-6361/202449345
Arnab Sarkar, Antonio C. Rodriguez, Sivan Ginzburg, L. Yungelson, C. Tout
Period bouncers are cataclysmic variables (CVs) that have evolved past their orbital period minimum. The strong disagreement between theory and observations of the relative fraction of period bouncers is a severe shortcoming in the understanding of CV evolution. We test the implications of the hypothesis that magnetic braking (MB), which is suggested to be an additional angular momentum loss (AML) mechanism for CVs below the period gap ($P_ orb 120$ min), weakens around their period minimum. We computed the evolution of CV donors below the period gap using the MESA code, assuming that the evolution of the system is driven by AML black due to gravitational wave radiation (GWR) and MB. We parametrised the MB strength as $ AML_ MB AML_ GWR black We computed two qualitatively different sets of models, one in which kappa is a constant and another in which kappa depends on stellar parameters in such a way that the value of kappa decreases as the CV approaches the period minimum ($P_ orb min), beyond which $ approx0$. We find that black two crucial effects drive the latter set of models. (1) A decrease in kappa as CVs approach the period minimum stalls their evolution so that they spend a long time in the observed period minimum spike ($80 P_ orb min Here, they become difficult to distinguish from pre-bounce systems in the spike. (2) A strong decrease in the mass-transfer rate makes them virtually undetectable as they evolve further. So, the CV stalls around the period minimum and then `disappears'. This reduces the number of detectable bouncers. Physical processes, such as dynamo action, white dwarf magnetism, and dead zones, may cause such a weakening of MB at short orbital periods. The weakening MB formalism black provides a possible solution to the problem of the dearth of black detectable period bouncers in CV observational surveys.
{"title":"Magnetic braking below the cataclysmic variable period gap and the observed dearth of period bouncers","authors":"Arnab Sarkar, Antonio C. Rodriguez, Sivan Ginzburg, L. Yungelson, C. Tout","doi":"10.1051/0004-6361/202449345","DOIUrl":"https://doi.org/10.1051/0004-6361/202449345","url":null,"abstract":"Period bouncers are cataclysmic variables (CVs) that have evolved past their orbital period minimum. The strong disagreement between theory and observations of the relative fraction of period bouncers is a severe shortcoming in the understanding of CV evolution. We test the implications of the hypothesis that magnetic braking (MB), which is suggested to be an additional angular momentum loss (AML) mechanism for CVs below the period gap ($P_ orb 120$ min), weakens around their period minimum. We computed the evolution of CV donors below the period gap using the MESA code, assuming that the evolution of the system is driven by AML black due to gravitational wave radiation (GWR) and MB. We parametrised the MB strength as $ AML_ MB AML_ GWR black We computed two qualitatively different sets of models, one in which kappa is a constant and another in which kappa depends on stellar parameters in such a way that the value of kappa decreases as the CV approaches the period minimum ($P_ orb min), beyond which $ approx0$. We find that black two crucial effects drive the latter set of models. (1) A decrease in kappa as CVs approach the period minimum stalls their evolution so that they spend a long time in the observed period minimum spike ($80 P_ orb min Here, they become difficult to distinguish from pre-bounce systems in the spike. (2) A strong decrease in the mass-transfer rate makes them virtually undetectable as they evolve further. So, the CV stalls around the period minimum and then `disappears'. This reduces the number of detectable bouncers. Physical processes, such as dynamo action, white dwarf magnetism, and dead zones, may cause such a weakening of MB at short orbital periods. The weakening MB formalism black provides a possible solution to the problem of the dearth of black detectable period bouncers in CV observational surveys.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":"32 24","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141354741","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-11DOI: 10.1051/0004-6361/202349122
L. Liberato, P. Tanga, David Mary, K. Minker, B. Carry, F. Spoto, P. Bartczak, Bruno Sicardy, D. Oszkiewicz, J. Desmars
Asteroids with companions constitute an excellent sample for studying the collisional and dynamical evolution of minor planets. The currently known binary population were discovered by different complementary techniques that produce, for the moment, a strongly biased distribution, especially in a range of intermediate asteroid sizes (approx 20 to 100 km) where both mutual photometric events and high-resolution adaptive optic imaging are poorly efficient. A totally independent technique of binary asteroid discovery, based on astrometry, can help to reveal new binary systems and populate a range of sizes and separations that remain nearly unexplored. In this work, we describe a dedicated period detection method and its results for the data set. This method looks for the presence of a periodic signature in the orbit post-fit residuals. After conservative filtering and validation based on statistical and physical criteria, we are able to present a first sample of astrometric binary candidates, to be confirmed by other observation techniques such as photometric light curves and stellar occultations.
{"title":"Binary asteroid candidates in Gaia DR3 astrometry","authors":"L. Liberato, P. Tanga, David Mary, K. Minker, B. Carry, F. Spoto, P. Bartczak, Bruno Sicardy, D. Oszkiewicz, J. Desmars","doi":"10.1051/0004-6361/202349122","DOIUrl":"https://doi.org/10.1051/0004-6361/202349122","url":null,"abstract":"Asteroids with companions constitute an excellent sample for studying the collisional and dynamical evolution of minor planets. The currently known binary population were discovered by different complementary techniques that produce, for the moment, a strongly biased distribution, especially in a range of intermediate asteroid sizes (approx 20 to 100 km) where both mutual photometric events and high-resolution adaptive optic imaging are poorly efficient. A totally independent technique of binary asteroid discovery, based on astrometry, can help to reveal new binary systems and populate a range of sizes and separations that remain nearly unexplored. In this work, we describe a dedicated period detection method and its results for the data set. This method looks for the presence of a periodic signature in the orbit post-fit residuals. After conservative filtering and validation based on statistical and physical criteria, we are able to present a first sample of astrometric binary candidates, to be confirmed by other observation techniques such as photometric light curves and stellar occultations.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":"9 8","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141355828","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-11DOI: 10.1051/0004-6361/202245680
Samata Das, R. Brose, M. Pohl, D. M. Meyer, I. Sushch
Context. In the core-collapse scenario, supernova remnants (SNRs) evolve inside complex wind-blown bubbles structured by massive progenitors during their lifetime. Therefore, particle acceleration and the emissions from these SNRs can carry the fingerprints of the evolutionary sequences of the progenitor stars. Aims. We investigate the impact of the ambient environment of core-collapse SNRs on particle spectra and emissions for two progenitors with different evolutionary tracks while accounting for the spatial transport of cosmic rays (CRs) and the magnetic turbulence that scatters CRs. Methods. We used the RATPaC sun sun $. We constructed the pre-supernova circumstellar medium (CSM) by solving the hydrodynamic equations for the lifetime of the progenitor stars. Then, the transport equation for cosmic rays, the magnetic turbulence in test-particle approximation, and the induction equation for the evolution of a large-scale magnetic field were solved simultaneously with the hydrodynamic equations for the expansion of SNRs inside the pre-supernova CSM in 1-D spherical symmetry. Results. sun $ progenitor, the spectral index reaches 2.4, even below $10 GeV sun $ progenitor, for which the spectral index becomes 2.2 only for a brief period during the interaction of SNR shock with the dense shell of red supergiant (RSG) wind material . At later stages of evolution, the spectra become soft above $ GeV sun $ progenitor is centre-filled at early stages, whereas that of the more massive progenitor is shell-like.
{"title":"Particle acceleration, escape, and non-thermal emission from core-collapse supernovae inside non-identical wind-blown bubbles","authors":"Samata Das, R. Brose, M. Pohl, D. M. Meyer, I. Sushch","doi":"10.1051/0004-6361/202245680","DOIUrl":"https://doi.org/10.1051/0004-6361/202245680","url":null,"abstract":"Context. In the core-collapse scenario, supernova remnants (SNRs) evolve inside complex wind-blown bubbles structured by massive progenitors during their lifetime. Therefore, particle acceleration and the emissions from these SNRs can carry the fingerprints of the evolutionary sequences of the progenitor stars. Aims. We investigate the impact of the ambient environment of core-collapse SNRs\u0000on particle spectra and emissions for two progenitors with different evolutionary tracks while accounting for the spatial transport of cosmic rays (CRs) and the magnetic turbulence that scatters CRs. Methods. We used the RATPaC sun sun $. We constructed the pre-supernova circumstellar medium (CSM) by solving the hydrodynamic equations for the lifetime of the progenitor stars. Then, the transport equation for cosmic rays, the magnetic turbulence in test-particle approximation, and the induction equation for the evolution of a large-scale magnetic field were solved simultaneously with the hydrodynamic equations for the expansion of SNRs inside the pre-supernova CSM in 1-D spherical symmetry. Results. sun $ progenitor, the spectral index reaches 2.4, even below $10 GeV sun $ progenitor, for which the spectral index becomes 2.2 only for a brief period during the interaction of SNR shock with the dense shell of red supergiant (RSG) wind material . At later stages of evolution, the spectra become soft above $ GeV sun $ progenitor is centre-filled at early stages, whereas that of the more massive progenitor is shell-like.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":"26 5","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141355510","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-11DOI: 10.1051/0004-6361/202449918
V. Ilyushin, H. Muller, M. Drozdovskaya, J. Jorgensen, S. Bauerecker, C. Maul, R. Porohovoi, E. Alekseev, O. Dorovskaya, O. Zakharenko, F. Lewen, S. Schlemmer, L.-H. Xu, R.M. Lees
We have started a measurement campaign of numerous methanol isotopologs in low-lying torsional states in order to provide extensive line lists for radio astronomical observations from an adequate spectroscopic model and to investigate how the intricate vibration-torsion-rotation interactions manifest themselves in the spectra of different isotopic species. After CD$_3$OH and CD$_3$OD, we turn our focus to CH$_3$OD, which is an important species for studying deuteration in prestellar cores and envelopes that enshroud protostars. Notably, deuteration is frequently viewed as a diagnostic tool for star formation. The measurements used in this study were obtained in two spectroscopic laboratories and cover large fractions of the 34 GHz$-$1.35 THz range. As done in previous studies, we employed a torsion-rotation Hamiltonian model for our analysis that is based on the rho-axis method. The resulting model describes the ground and first excited torsional states of CH$_3$OD well up to quantum numbers $J 51$ and $K_a 18$. We derived a line list for radio astronomical observations from this model that is accurate up to at least 1.35 THz and should be sufficient for all types of radio astronomical searches for this methanol isotopolog in these two lowest torsional states. This line list was applied to a reinvestigation of CH$_3$OD in data from the Protostellar Interferometric Line Survey of IRAS 16293$-$2422 obtained with the Atacama Large Millimeter/submillimeter Array. The new accurately determined value for the column density of CH$_3$OD implies that the deuteration in methanol differs in its two functional groups by a factor of sim 7.5.
{"title":"Rotational spectroscopy of CH$_3$OD with a reanalysis of CH_3OD toward IRAS 16293-2422","authors":"V. Ilyushin, H. Muller, M. Drozdovskaya, J. Jorgensen, S. Bauerecker, C. Maul, R. Porohovoi, E. Alekseev, O. Dorovskaya, O. Zakharenko, F. Lewen, S. Schlemmer, L.-H. Xu, R.M. Lees","doi":"10.1051/0004-6361/202449918","DOIUrl":"https://doi.org/10.1051/0004-6361/202449918","url":null,"abstract":"We have started a measurement campaign of numerous methanol isotopologs in low-lying torsional states \u0000in order to provide extensive line lists for radio astronomical observations from an adequate \u0000spectroscopic model and to investigate how the intricate vibration-torsion-rotation interactions \u0000manifest themselves in the spectra of different isotopic species. \u0000After CD$_3$OH and CD$_3$OD, we turn our focus to CH$_3$OD, which is an important species \u0000 for studying deuteration in prestellar cores and envelopes that enshroud protostars. \u0000Notably, deuteration is frequently viewed as a diagnostic tool for star formation. The measurements used in this study were obtained in two spectroscopic laboratories and cover large fractions \u0000of the 34 GHz$-$1.35 THz range. As done in previous studies, we employed a torsion-rotation Hamiltonian model for our analysis that is based on the rho-axis method. \u0000The resulting model describes the ground and first excited torsional states of CH$_3$OD well \u0000up to quantum numbers $J 51$ and $K_a 18$. We derived a line list for radio astronomical observations from this model that is accurate up to at least 1.35 THz and should be sufficient for all types of radio astronomical searches for this methanol isotopolog in these two lowest torsional states. This line list was applied to a reinvestigation of CH$_3$OD in data from the Protostellar Interferometric Line Survey of IRAS 16293$-$2422 obtained with the Atacama Large Millimeter/submillimeter Array. The new accurately determined value for the column density of CH$_3$OD implies that the deuteration in methanol differs in its two functional groups by a factor of sim 7.5.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":"74 5","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141359641","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-10DOI: 10.1051/0004-6361/202450592
X. Rodrigues, M. Karl, P. Padovani, P. Giommi, S. Paiano, Renato Falomo, M. Petropoulou, F. Oikonomou
A correlation has been reported between the arrival directions of high-energy IceCube events and gamma -ray blazars classified as intermediate- and high-synchrotron-peaked BL Lacs. Subsequent studies have investigated the optical properties of these sources, compiled and analyzed public multiwavelength data, and constrained their individual neutrino emission based on public IceCube point-source data. We provide a theoretical interpretation of public multiwavelength and neutrino point source data for the 32 BL Lac objects in the sample previously associated with an IceCube alert event. We combined the individual source results to draw conclusions regarding the multimesssenger properties of the sample and the required power in relativistic protons. We performed particle interaction modeling using open-source numerical simulation software. We constrained the model parameters using a novel and unique approach that simultaneously describes the host galaxy contribution, the observed synchrotron peak properties, the average multiwavelength fluxes, and, where possible, the IceCube point source constraints. We show that a single-zone leptohadronic model can describe the multiwavelength broadband fluxes from all 32 IceCube candidates. In some cases, the model suggests that hadronic emission may contribute a considerable fraction of the gamma -ray flux. The required power in relativistic protons ranges from a few percent to a factor of ten of the Eddington luminosity, which is energetically less demanding compared to other leptohadronic blazar models in recent literature. The model can describe the 68 confidence level IceCube flux for a large fraction of the masquerading BL Lacs in the sample, including TXS 0506+056; whereas, for true BL Lacs, the model predicts a low neutrino flux in the IceCube sensitivity range. Physically, this distinction is due to the presence of photons from broad line emission in masquerading BL Lacs, which increase the efficiency of hadronic interactions. The predicted neutrino flux peaks between a few petaelectronvolt and 100 PeV and scales positively with the flux in the gigaelectronvolt, megaelectronvolt, X-ray, and optical bands. Based on these results, we provide a list of the brightest neutrino emitters, which can be used for future searches targeting the 10-100 PeV regime.
{"title":"The Spectra of IceCube Neutrino (SIN) candidate sources. V. Modeling and interpretation of multiwavelength and neutrino data","authors":"X. Rodrigues, M. Karl, P. Padovani, P. Giommi, S. Paiano, Renato Falomo, M. Petropoulou, F. Oikonomou","doi":"10.1051/0004-6361/202450592","DOIUrl":"https://doi.org/10.1051/0004-6361/202450592","url":null,"abstract":"A correlation has been reported between the arrival directions of high-energy IceCube events and gamma -ray blazars classified as intermediate- and high-synchrotron-peaked BL Lacs. Subsequent studies have investigated the optical properties of these sources, compiled and analyzed public multiwavelength data, and constrained their individual neutrino emission based on public IceCube point-source data. We provide a theoretical interpretation of public multiwavelength and neutrino point source data for the 32 BL Lac objects in the sample previously associated with an IceCube alert event. We combined the individual source results to draw conclusions regarding the multimesssenger properties of the sample and the required power in relativistic protons. We performed particle interaction modeling using open-source numerical simulation software. We constrained the model parameters using a novel and unique approach that simultaneously describes the host galaxy contribution, the observed synchrotron peak properties, the average multiwavelength fluxes, and, where possible, the IceCube point source constraints. We show that a single-zone leptohadronic model can describe the multiwavelength broadband fluxes from all 32 IceCube candidates. In some cases, the model suggests that hadronic emission may contribute a considerable fraction of the gamma -ray flux. The required power in relativistic protons ranges from a few percent to a factor of ten of the Eddington luminosity, which is energetically less demanding compared to other leptohadronic blazar models in recent literature. The model can describe the 68 confidence level IceCube flux for a large fraction of the masquerading BL Lacs in the sample, including TXS 0506+056; whereas, for true BL Lacs, the model predicts a low neutrino flux in the IceCube sensitivity range. Physically, this distinction is due to the presence of photons from broad line emission in masquerading BL Lacs, which increase the efficiency of hadronic interactions. The predicted neutrino flux peaks between a few petaelectronvolt and 100 PeV and scales positively with the flux in the gigaelectronvolt, megaelectronvolt, X-ray, and optical bands. Based on these results, we provide a list of the brightest neutrino emitters, which can be used for future searches targeting the 10-100 PeV regime.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":"116 14","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141361139","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-10DOI: 10.1051/0004-6361/202449556
N. Raycheva, M. Haverkorn, S. Ideguchi, J. Stil, X. Sun, J. L. Han, E. Carretti, X. Y. Gao, A. Bracco, S. E. Clark, J. M. Dickey, B. Gaensler, A. Hill, T. Landecker, A. Ordog, A. Seta, M. Tahani, M. Wolleben
Faraday tomography of broadband radio polarization surveys enables us to study magnetic fields and their interaction with the interstellar medium (ISM). Such surveys include the Global Magneto-Ionic Medium Survey (GMIMS), which covers the northern and southern hemispheres at sim 300--1800 MHz. In this work, we used the GMIMS High Band South (1328--1768 MHz), also named the Southern Twenty-centimeter All-sky Polarization Survey (STAPS), which observes the southern sky at a resolution of 18arcmin . To extract the key parameters of the magnetized ISM from STAPS, we computed the Faraday moments of the tomographic data cubes. These moments include the total polarized intensity, the mean Faraday depth weighted by the polarized intensity, the weighted dispersion of the Faraday spectrum, and its skewness. We compared the Faraday moments to those calculated over the same frequency range in the northern sky (using the Dominion Radio Astrophysical Observatory, DRAO), in a strip of $360 that overlaps with STAPS coverage. We find that the total polarized intensity is generally dominated by diffuse emission that decreases at longitudes of $l The Faraday moments reveal a variety of polarization structures. Low-intensity regions at high latitudes usually have a single Faraday depth component. Due to its insufficiently large frequency coverage, STAPS cannot detect Faraday thick structures. Comparing the Faraday depths from STAPS to total rotation measures from extragalactic sources suggests that STAPS frequencies are high enough that the intervening ISM causes depolarization to background emission at intermediate and high Galactic latitudes. Where they overlap, the STAPS and DRAO surveys exhibit broad correspondence but differ in polarized intensity by a factor of sim 1.8.
{"title":"Faraday moments of the Southern Twenty-centimeter All-sky Polarization Survey (STAPS)","authors":"N. Raycheva, M. Haverkorn, S. Ideguchi, J. Stil, X. Sun, J. L. Han, E. Carretti, X. Y. Gao, A. Bracco, S. E. Clark, J. M. Dickey, B. Gaensler, A. Hill, T. Landecker, A. Ordog, A. Seta, M. Tahani, M. Wolleben","doi":"10.1051/0004-6361/202449556","DOIUrl":"https://doi.org/10.1051/0004-6361/202449556","url":null,"abstract":"Faraday tomography of broadband radio polarization surveys enables us to study magnetic fields and their interaction with the interstellar medium (ISM). Such surveys include the Global Magneto-Ionic Medium Survey (GMIMS), which covers the northern and southern hemispheres at sim 300--1800 MHz. In this work, we used the GMIMS High Band South (1328--1768 MHz), also named the Southern Twenty-centimeter All-sky Polarization Survey (STAPS), which observes the southern sky at a resolution of 18arcmin . To extract the key parameters of the magnetized ISM from STAPS, we computed the Faraday moments of the tomographic data cubes. These moments include the total polarized intensity, the mean Faraday depth weighted by the polarized intensity, the weighted dispersion of the Faraday spectrum, and its skewness. We compared the Faraday moments to those calculated over the same frequency range in the northern sky (using the Dominion Radio Astrophysical Observatory, DRAO), in a strip of $360 that overlaps with STAPS coverage. We find that the total polarized intensity is generally dominated by diffuse emission that decreases at longitudes of $l The Faraday moments reveal a variety of polarization structures. Low-intensity regions at high latitudes usually have a single Faraday depth component. Due to its insufficiently large frequency coverage, STAPS cannot detect Faraday thick structures. Comparing the Faraday depths from STAPS to total rotation measures from extragalactic sources suggests that STAPS frequencies are high enough that the intervening ISM causes depolarization to background emission at intermediate and high Galactic latitudes. Where they overlap, the STAPS and DRAO surveys exhibit broad correspondence but differ in polarized intensity by a factor of sim 1.8.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":" 655","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141364297","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-10DOI: 10.1051/0004-6361/202349031
M. Kluge, J. Comparat, A. Liu, F. Balzer, E. Bulbul, J. Ider Chitham, V. Ghirardini, C. Garrel, Y. Bahar, E. Artis, R. Bender, N. Clerc, T. Dwelly, M. Fabricius, S. Grandis, D. Hernandez-Lang, G. J. Hill, J. Joshi, G. Lamer, A. Merloni, K. Nandra, F. Pacaud, P. Predehl, M. Ramos-Ceja, T. Reiprich, M. Salvato, J. Sanders, T. Schrabback, R. Seppi, S. Zelmer, A. Zenteno, X. Zhang
The first SRG/ All-Sky Survey ( provides the largest intracluster medium-selected galaxy cluster and group catalog covering the western Galactic hemisphere. Compared to samples selected purely on X-ray extent, the sample purity can be enhanced by identifying cluster candidates using optical and near-infrared data from the DESI Legacy Imaging Surveys. Using the red-sequence-based cluster finder we measured individual photometric properties (redshift $z_ richness lambda , optical center, and BCG position) for 12,000 clusters over a sky area of 13,116,deg$^2$, augmented by 247 cases identified by matching the candidates with known clusters from the literature. The median redshift of the identified sample is $z=0.31$, with 10 of the clusters at $z>0.72$. The photometric redshifts have an accuracy of $ z/(1+z) for $0.05 and optical completeness >95 for $z>0.05$. For these and further quality assessments of the identified catalog, we applied our identification method to a collection of galaxy cluster catalogs in the literature, as well as blindly on the full Legacy Surveys covering 24,069,deg$^2$. Using a combination of these cluster samples, we investigated the velocity dispersion-richness relation, finding that it scales with richness as $ norm with an intrinsic scatter of $ in The primary product of our work is the identified cluster catalog with high purity and a well-defined X-ray selection process, opening the path for precise cosmological analyses presented in companion papers.
{"title":"The SRG/eROSITA All-Sky Survey. Optical identification and properties of galaxy clusters and groups in thewestern galactic hemisphere","authors":"M. Kluge, J. Comparat, A. Liu, F. Balzer, E. Bulbul, J. Ider Chitham, V. Ghirardini, C. Garrel, Y. Bahar, E. Artis, R. Bender, N. Clerc, T. Dwelly, M. Fabricius, S. Grandis, D. Hernandez-Lang, G. J. Hill, J. Joshi, G. Lamer, A. Merloni, K. Nandra, F. Pacaud, P. Predehl, M. Ramos-Ceja, T. Reiprich, M. Salvato, J. Sanders, T. Schrabback, R. Seppi, S. Zelmer, A. Zenteno, X. Zhang","doi":"10.1051/0004-6361/202349031","DOIUrl":"https://doi.org/10.1051/0004-6361/202349031","url":null,"abstract":"The first SRG/ All-Sky Survey ( provides the largest intracluster medium-selected galaxy cluster and group catalog covering the western Galactic hemisphere. Compared to samples selected purely on X-ray extent, the sample purity can be enhanced by identifying cluster candidates using optical and near-infrared data from the DESI Legacy Imaging Surveys. Using the red-sequence-based cluster finder we measured individual photometric properties (redshift $z_ richness lambda , optical center, and BCG position) for 12,000 clusters over a sky area of 13,116,deg$^2$, augmented by 247 cases identified by matching the candidates with known clusters from the literature. The median redshift of the identified sample is $z=0.31$, with 10<!PCT!> of the clusters at $z>0.72$. The photometric redshifts have an accuracy of $ z/(1+z) for $0.05<z<0.9$. Spectroscopic cluster properties (redshift spec $ and velocity dispersion sigma ) were measured a posteriori for a subsample of 3210 and 1499 clusters, respectively, using an extensive compilation of spectroscopic redshifts of galaxies from the literature. We infer that the primary sample has a purity of 86<!PCT!> and optical completeness >95<!PCT!> for $z>0.05$. For these and further quality assessments of the identified catalog, we applied our identification method to a collection of galaxy cluster catalogs in the literature, as well as blindly on the full Legacy Surveys covering 24,069,deg$^2$. Using a combination of these cluster samples, we investigated the velocity dispersion-richness relation, finding that it scales with richness as $ norm with an intrinsic scatter of $ in The primary product of our work is the identified cluster catalog with high purity and a well-defined X-ray selection process, opening the path for precise cosmological analyses presented in companion papers.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":"114 30","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141361862","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-10DOI: 10.1051/0004-6361/202449726
J. Escudero Pedrosa, I. Agudo, Till Moritz, P. Alan Marscher, S. Jorstad, A. Tramacere, C. Casadio, C. Thum, I. Myserlis, A. Sievers, J. Otero-Santos, D. Morcuende, R. López-Coto, F. D’Ammando, G. Bonnoli, M. Gurwell, José Luis Gómez, R. Rao, G. Keating
The blazar AO 0235+164 located at redshift $z=0.94$, has displayed interesting and repeating flaring activity in the past, with recent episodes in 2008 and 2015. In 2020, the source brightened again, starting a new flaring episode that peaked in 2021. We study the origin and properties of the 2021 flare in relation to previous studies and the historical behavior of the source, in particular the 2008 and 2015 flaring episodes. We analyzed the multiwavelength photo-polarimetric evolution of the source. From Very Long Baseline Array images, we derived the kinematic parameters of new components associated with the 2021 flare. We used this information to constrain a model for the spectral energy distribution of the emission during the flaring period. We propose an analytical geometric model to test whether the observed wobbling of the jet is consistent with precession. We report the appearance of two new components that are ejected in a different direction than previously, confirming the wobbling of the jet. We find that the direction of ejection is consistent with that of a precessing jet. Our derived period independently agrees with the values commonly found in the literature. Modeling of the spectral energy distribution further confirms that the differences between flares can be attributed to geometrical effects.
{"title":"The flaring activity of blazar AO 0235+164 in 2021","authors":"J. Escudero Pedrosa, I. Agudo, Till Moritz, P. Alan Marscher, S. Jorstad, A. Tramacere, C. Casadio, C. Thum, I. Myserlis, A. Sievers, J. Otero-Santos, D. Morcuende, R. López-Coto, F. D’Ammando, G. Bonnoli, M. Gurwell, José Luis Gómez, R. Rao, G. Keating","doi":"10.1051/0004-6361/202449726","DOIUrl":"https://doi.org/10.1051/0004-6361/202449726","url":null,"abstract":"The blazar AO 0235+164 located at redshift $z=0.94$, has displayed interesting and repeating flaring activity in the past, with recent episodes in 2008 and 2015. In 2020, the source brightened again, starting a new flaring episode that peaked in 2021. We study the origin and properties of the 2021 flare in relation to previous studies and the historical behavior of the source, in particular the 2008 and 2015 flaring episodes. We analyzed the multiwavelength photo-polarimetric evolution of the source. From Very Long Baseline Array images, we derived the kinematic parameters of new components associated with the 2021 flare. We used this information to constrain a model for the spectral energy distribution of the emission during the flaring period. We propose an analytical geometric model to test whether the observed wobbling of the jet is consistent with precession. We report the appearance of two new components that are ejected in a different direction than previously, confirming the wobbling of the jet. We find that the direction of ejection is consistent with that of a precessing jet.\u0000 Our derived period independently agrees with the values commonly found in the literature.\u0000 \u0000 Modeling of the spectral energy distribution further confirms that the differences between flares can be attributed to geometrical effects.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":" 82","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-06-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141365512","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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