ABSTRACT Radio blazars have been linked both to individual high-energy neutrino events and to excesses in likelihood sky maps constructed from lower-energy neutrino data. However, the exact mechanism by which neutrinos are produced in these sources is still unknown. Here, we demonstrate that IceCube neutrinos with energies over 200 TeV, which were previously associated with bright radio blazars, are significantly more likely to be accompanied by flares of lower-energy events, compared to those lacking blazar counterparts. The parsec-scale core radio flux density of blazars, positioned within the error regions of energetic events, is strongly correlated with the likelihood of a day-scale lower-energy neutrino flare in directional and temporal coincidence with the high-energy event, reported by IceCube. The probability of a chance correlation is 3.6 × 10−4. This confirms the neutrino-blazar connection in a new and independent way, and provides valuable clues to understanding the origin of astrophysical neutrinos.
{"title":"Neutrino flares of radio blazars observed from TeV to PeV","authors":"Alisa Suray, Sergey Troitsky","doi":"10.1093/mnrasl/slad136","DOIUrl":"https://doi.org/10.1093/mnrasl/slad136","url":null,"abstract":"ABSTRACT Radio blazars have been linked both to individual high-energy neutrino events and to excesses in likelihood sky maps constructed from lower-energy neutrino data. However, the exact mechanism by which neutrinos are produced in these sources is still unknown. Here, we demonstrate that IceCube neutrinos with energies over 200 TeV, which were previously associated with bright radio blazars, are significantly more likely to be accompanied by flares of lower-energy events, compared to those lacking blazar counterparts. The parsec-scale core radio flux density of blazars, positioned within the error regions of energetic events, is strongly correlated with the likelihood of a day-scale lower-energy neutrino flare in directional and temporal coincidence with the high-energy event, reported by IceCube. The probability of a chance correlation is 3.6 × 10−4. This confirms the neutrino-blazar connection in a new and independent way, and provides valuable clues to understanding the origin of astrophysical neutrinos.","PeriodicalId":18951,"journal":{"name":"Monthly Notices of the Royal Astronomical Society: Letters","volume":"122 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134960393","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}
ABSTRACT It has been hypothesized that dark matter is comprised of ultra-light bosons whose collective phenomena can be described as a scalar field undergoing coherent oscillations. Examples include axion and fuzzy dark matter models. In this ultra-light dark matter (ULDM) scenario, the harmonic variation in the field’s energy–momentum tensor sources an oscillating component of the gravitational potential that we show can resonantly excite stellar oscillations. A mathematical framework for predicting the amplitude of these oscillations is developed, which reveals that ULDM predominantly excites p-modes of degree l = 1. An investigation of resonantly excited solar oscillations is presented, from which we conclude that dark matter induced oscillations of the Sun are likely undetectable. We discuss prospects for constraining ULDM using other stellar objects.
{"title":"Dark matter-induced stellar oscillations","authors":"Jeremy Sakstein, Ippocratis D Saltas","doi":"10.1093/mnrasl/slad133","DOIUrl":"https://doi.org/10.1093/mnrasl/slad133","url":null,"abstract":"ABSTRACT It has been hypothesized that dark matter is comprised of ultra-light bosons whose collective phenomena can be described as a scalar field undergoing coherent oscillations. Examples include axion and fuzzy dark matter models. In this ultra-light dark matter (ULDM) scenario, the harmonic variation in the field’s energy–momentum tensor sources an oscillating component of the gravitational potential that we show can resonantly excite stellar oscillations. A mathematical framework for predicting the amplitude of these oscillations is developed, which reveals that ULDM predominantly excites p-modes of degree l = 1. An investigation of resonantly excited solar oscillations is presented, from which we conclude that dark matter induced oscillations of the Sun are likely undetectable. We discuss prospects for constraining ULDM using other stellar objects.","PeriodicalId":18951,"journal":{"name":"Monthly Notices of the Royal Astronomical Society: Letters","volume":"48 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136061949","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}
ABSTRACT We present clear and direct evidence of the pre-processing effect of group galaxies falling into clusters in the local Universe (z ≲ 0.1). We start with a sample of 238 clusters, from which we select 153 with N200 ≥ 20. We considered 1641 groups within the turnaround radius (∼5 × R200) of these 153 clusters. There are 6654 individual cluster galaxies and 4133 group galaxies within this radius. We considered two control samples of galaxies, in isolated groups and in the field. The former comprises 2601 galaxies within 1606 isolated groups, and the latter has 4273 field objects. The fraction of star-forming galaxies in infalling groups has a distinct clustercentric behaviour in comparison to the remaining cluster galaxies. Even at 5 × R200 the group galaxies already show a reduced fraction of star-forming objects. At this radius, the results for the individual cluster galaxies are actually compatible with the field. That is strong evidence that the group environment is effective to quench the star formation prior to the cluster arrival. The group star-forming fraction remains roughly constant inwards, decreasing significantly only within the cluster R200 radius. We have also found that the pre-processing effect depends on the group mass (indicated by the number of members). The effect is larger for more massive groups. However, it is significant even for pairs and triplets. Finally, we find evidence that the time-scale required for morphological transformation is larger than the one for quenching.
{"title":"The Role of Groups in Galaxy Evolution: compelling evidence of pre-processing out to the turnaround radius of clusters","authors":"Lopes, P. A. A., Ribeiro, A. L. B., Brambila, D.","doi":"10.1093/mnrasl/slad134","DOIUrl":"https://doi.org/10.1093/mnrasl/slad134","url":null,"abstract":"ABSTRACT We present clear and direct evidence of the pre-processing effect of group galaxies falling into clusters in the local Universe (z ≲ 0.1). We start with a sample of 238 clusters, from which we select 153 with N200 ≥ 20. We considered 1641 groups within the turnaround radius (∼5 × R200) of these 153 clusters. There are 6654 individual cluster galaxies and 4133 group galaxies within this radius. We considered two control samples of galaxies, in isolated groups and in the field. The former comprises 2601 galaxies within 1606 isolated groups, and the latter has 4273 field objects. The fraction of star-forming galaxies in infalling groups has a distinct clustercentric behaviour in comparison to the remaining cluster galaxies. Even at 5 × R200 the group galaxies already show a reduced fraction of star-forming objects. At this radius, the results for the individual cluster galaxies are actually compatible with the field. That is strong evidence that the group environment is effective to quench the star formation prior to the cluster arrival. The group star-forming fraction remains roughly constant inwards, decreasing significantly only within the cluster R200 radius. We have also found that the pre-processing effect depends on the group mass (indicated by the number of members). The effect is larger for more massive groups. However, it is significant even for pairs and triplets. Finally, we find evidence that the time-scale required for morphological transformation is larger than the one for quenching.","PeriodicalId":18951,"journal":{"name":"Monthly Notices of the Royal Astronomical Society: Letters","volume":"87 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136061911","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}
J. L. Ortiz, M. Kretlow, C. Schnabel, N. Morales, J. Flores-Mart'in, M. S. Gonz'alez, F. Casarramona, A. Selva, C. Perell'o, A. Rom'an-Reche, S. Alonso, J. Rizos, R. Gonccalves, A. Castillo, J. Madiedo, P. M. S'anchez, J. M. F. and'ujar, J. L. Maestre, E. Smith, M. Gil, V. Pelenjow, S. M. Soriano, J. Mart'i, P. Luque-Escamilla, R. Casas, J. D. Casal, J. Rovira, F. Aceituno, V. Dekert, V. D. O. Guimer'a, J. Estepa, Y. Kilic, Rodrigo Leiva, P. Santos-Sanz, R. Duffard, E. Fern'andez-Valenzuela, M. Vara-Lubiano, A. Alvarez-Candal, F. Rommel
On 12 December 2023, the star α Orionis will be occulted by asteroid (319) Leona. This represents an extraordinary and unique opportunity to analyze the brightness distribution of Betelgeuse’s photosphere with extreme angular resolution by studying lightcurves from different points on Earth and at different wavelengths. Here we present observations of another occultation by asteroid Leona, on 13 September 2023, whose goal was to determine Leona’s projected shape and size in preparation for the December 12th event and its interpretation. The occultation campaign was highly successful with 25 positive detections from 17 different sites and a near miss. The effective diameter in projected area derived from the positive detections was 66 ± 2 km using an elliptical fit to the instantaneous limb. The body is highly elongated, with dimensions of 79.6 ± 2.2 km x 54.8 ± 1.3 km in its long and short axis, respectively, at occultation time. This result, in combination with dense time series photometry of Leona that we recently obtained, together with archival sparse photometry, allowed us to predict the angular size of the asteroid for the Betelgeuse event and to simulate the expected brightness change. Also, an accurate position coming from the occultation is provided, to improve the orbit of Leona.
{"title":"The stellar occultation by (319) Leona on 13 September 2023 in preparation for the occultation of Betelgeuse","authors":"J. L. Ortiz, M. Kretlow, C. Schnabel, N. Morales, J. Flores-Mart'in, M. S. Gonz'alez, F. Casarramona, A. Selva, C. Perell'o, A. Rom'an-Reche, S. Alonso, J. Rizos, R. Gonccalves, A. Castillo, J. Madiedo, P. M. S'anchez, J. M. F. and'ujar, J. L. Maestre, E. Smith, M. Gil, V. Pelenjow, S. M. Soriano, J. Mart'i, P. Luque-Escamilla, R. Casas, J. D. Casal, J. Rovira, F. Aceituno, V. Dekert, V. D. O. Guimer'a, J. Estepa, Y. Kilic, Rodrigo Leiva, P. Santos-Sanz, R. Duffard, E. Fern'andez-Valenzuela, M. Vara-Lubiano, A. Alvarez-Candal, F. Rommel","doi":"10.1093/mnrasl/slad179","DOIUrl":"https://doi.org/10.1093/mnrasl/slad179","url":null,"abstract":"On 12 December 2023, the star α Orionis will be occulted by asteroid (319) Leona. This represents an extraordinary and unique opportunity to analyze the brightness distribution of Betelgeuse’s photosphere with extreme angular resolution by studying lightcurves from different points on Earth and at different wavelengths. Here we present observations of another occultation by asteroid Leona, on 13 September 2023, whose goal was to determine Leona’s projected shape and size in preparation for the December 12th event and its interpretation. The occultation campaign was highly successful with 25 positive detections from 17 different sites and a near miss. The effective diameter in projected area derived from the positive detections was 66 ± 2 km using an elliptical fit to the instantaneous limb. The body is highly elongated, with dimensions of 79.6 ± 2.2 km x 54.8 ± 1.3 km in its long and short axis, respectively, at occultation time. This result, in combination with dense time series photometry of Leona that we recently obtained, together with archival sparse photometry, allowed us to predict the angular size of the asteroid for the Betelgeuse event and to simulate the expected brightness change. Also, an accurate position coming from the occultation is provided, to improve the orbit of Leona.","PeriodicalId":18951,"journal":{"name":"Monthly Notices of the Royal Astronomical Society: Letters","volume":"24 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-09-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139338045","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}
Although the present-day orbital distribution of minor bodies that go around the Sun between the orbit of Neptune and the Kuiper Cliff is well understood, past ~50 au from the Sun, our vision gets blurred as objects become fainter and fainter and their orbital periods span several centuries. Deep imaging using the largest telescopes can overcome the first issue but the problems derived from the second one are better addressed using data analysis techniques. Here, we make use of the heliocentric range and range-rate of the known Kuiper belt objects and their uncertainties to identify structures in orbital parameter space beyond the Kuiper Cliff. The distribution in heliocentric range there closely resembles that of the outer main asteroid belt with a gap at 70 au that may signal the existence of a dynamical analogue of the Jupiter family comets. Outliers in the distribution of mutual nodal distances suggest that a massive perturber is present beyond the heliopause.
{"title":"Past the outer rim, into the unknown: Structures beyond the Kuiper Cliff","authors":"Marcos, C. de la Fuente, Marcos, R. de la Fuente","doi":"10.1093/mnrasl/slad132","DOIUrl":"https://doi.org/10.1093/mnrasl/slad132","url":null,"abstract":"Although the present-day orbital distribution of minor bodies that go around the Sun between the orbit of Neptune and the Kuiper Cliff is well understood, past ~50 au from the Sun, our vision gets blurred as objects become fainter and fainter and their orbital periods span several centuries. Deep imaging using the largest telescopes can overcome the first issue but the problems derived from the second one are better addressed using data analysis techniques. Here, we make use of the heliocentric range and range-rate of the known Kuiper belt objects and their uncertainties to identify structures in orbital parameter space beyond the Kuiper Cliff. The distribution in heliocentric range there closely resembles that of the outer main asteroid belt with a gap at 70 au that may signal the existence of a dynamical analogue of the Jupiter family comets. Outliers in the distribution of mutual nodal distances suggest that a massive perturber is present beyond the heliopause.","PeriodicalId":18951,"journal":{"name":"Monthly Notices of the Royal Astronomical Society: Letters","volume":"16 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136129917","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}
Nonlinear pulsation modeling of classical variable stars is among the first topics which were developed at the beginning of the computational era. Various developments were made, and many questions were answered in the past 60 years, and the models became more complex, describing the genuinely 3D convection in a single dimension. Despite its successes, the recent public availability of the MESA Radial Stellar Pulsations (MESA RSP) module and the emerging results from multidimensional codes made clear that the 8 free convective parameters, unique to these models, together with the underlying physical models need calibration. This could be done by comparing them against multi-dimensional codes, but before that, it is important to scrutinize the free parameters of the 1D codes using observations. This is a follow-up work of our previous calibration on the convective parameters of the Budapest-Florida and MESA RSP pulsation codes for RRab stars. In this paper, we extend the previous calibration to the RRc stars and the RR Lyrae stars in general. We found that correlations of some of the parameters are present in RRc stars as well but have a different nature, while high-temperature RRc stars' pulsation properties are very sensitive to the chosen parameter sets.
{"title":"Temperature dependent convective parameters for RRc 1D-models","authors":"Kovács, Gábor B., Nuspl, János, Szabó, Róbert","doi":"10.1093/mnrasl/slad131","DOIUrl":"https://doi.org/10.1093/mnrasl/slad131","url":null,"abstract":"Nonlinear pulsation modeling of classical variable stars is among the first topics which were developed at the beginning of the computational era. Various developments were made, and many questions were answered in the past 60 years, and the models became more complex, describing the genuinely 3D convection in a single dimension. Despite its successes, the recent public availability of the MESA Radial Stellar Pulsations (MESA RSP) module and the emerging results from multidimensional codes made clear that the 8 free convective parameters, unique to these models, together with the underlying physical models need calibration. This could be done by comparing them against multi-dimensional codes, but before that, it is important to scrutinize the free parameters of the 1D codes using observations. This is a follow-up work of our previous calibration on the convective parameters of the Budapest-Florida and MESA RSP pulsation codes for RRab stars. In this paper, we extend the previous calibration to the RRc stars and the RR Lyrae stars in general. We found that correlations of some of the parameters are present in RRc stars as well but have a different nature, while high-temperature RRc stars' pulsation properties are very sensitive to the chosen parameter sets.","PeriodicalId":18951,"journal":{"name":"Monthly Notices of the Royal Astronomical Society: Letters","volume":"11 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135109777","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}
G. Galazutdinov, R. Baluev, G. Valyavin, V. Aitov, D. Gadelshin, A. Valeev, E. Sendzikas, E. Sokov, G. Mitiani, T. Burlakova, I. Yakunin, K. Antonyuk, V. Vlasyuk, I. Romanyuk, A. Rzaev, M. Yushkin, A. Ivanova, A. Tavrov, O. Korablev
We report an independent Doppler confirmation of the TESS planet candidate orbiting an F-type main sequence star TOI-1408 located 140 pc away. We present a set of radial velocities obtained with a high-resolution fiber-optic spectrograph FFOREST mounted at the SAO RAS 6-m telescope (BTA-6). Our self- consistent analysis of these Doppler data and TESS photometry suggests a grazing transit such that the planet obscures its host star by only a portion of the visible disc. Because of this degeneracy, the radius of TOI-1408.01 appears ill-determined with lower limit about ∼1 RJup, significantly larger than in the current TESS solution. We also derive the planet mass of 1.69 ± 0.20 MJup and the orbital period ∼4.425 days, thus making this object a typical hot Jupiter, but with a significant orbital eccentricity of 0.259 ± 0.026. Our solution may suggest the planet is likely to experience a high tidal eccentricity migration at the stage of intense orbital rounding, or may indicate possible presence of other unseen companions in the system, yet to be detected.
{"title":"Doppler confirmation of TESS planet candidate TOI1408.01: grazing transit and likely eccentric orbit","authors":"G. Galazutdinov, R. Baluev, G. Valyavin, V. Aitov, D. Gadelshin, A. Valeev, E. Sendzikas, E. Sokov, G. Mitiani, T. Burlakova, I. Yakunin, K. Antonyuk, V. Vlasyuk, I. Romanyuk, A. Rzaev, M. Yushkin, A. Ivanova, A. Tavrov, O. Korablev","doi":"10.1093/mnrasl/slad127","DOIUrl":"https://doi.org/10.1093/mnrasl/slad127","url":null,"abstract":"\u0000 We report an independent Doppler confirmation of the TESS planet candidate orbiting an F-type main sequence star TOI-1408 located 140 pc away. We present a set of radial velocities obtained with a high-resolution fiber-optic spectrograph FFOREST mounted at the SAO RAS 6-m telescope (BTA-6). Our self- consistent analysis of these Doppler data and TESS photometry suggests a grazing transit such that the planet obscures its host star by only a portion of the visible disc. Because of this degeneracy, the radius of TOI-1408.01 appears ill-determined with lower limit about ∼1 RJup, significantly larger than in the current TESS solution. We also derive the planet mass of 1.69 ± 0.20 MJup and the orbital period ∼4.425 days, thus making this object a typical hot Jupiter, but with a significant orbital eccentricity of 0.259 ± 0.026. Our solution may suggest the planet is likely to experience a high tidal eccentricity migration at the stage of intense orbital rounding, or may indicate possible presence of other unseen companions in the system, yet to be detected.","PeriodicalId":18951,"journal":{"name":"Monthly Notices of the Royal Astronomical Society: Letters","volume":"90 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"85651635","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}
Gravitational waves (GWs) from binary black hole mergers provide unique opportunities for cosmological inference such as standard sirens. However, the accurate determination of the luminosity distance of the event is limited by the correlation between the distance and the angle between the binary's orbital angular momentum and the observer's line of sight. In the letter, we investigate the effect of precession on the distance estimation of binary black hole events for the third-generation (3G) GW detectors. We find that the precession can enhance the precision of distance inference by one order of magnitude compared to the scenario where precession is absent. The constraint on the host galaxies can be improved due to the improved distance measurement, therefore the Hubble constant can be measured with higher precision and accuracy. These findings underscore the noteworthy impact of precession on the precision of distance estimation for 3G ground-based GW detectors, which can serve as highly accurate probes of the Universe.
{"title":"Precessing binary black holes as better dark sirens","authors":"Qianyun Yun, Wen-Biao Han, Qian Hu, Haiguang Xu","doi":"10.1093/mnrasl/slad119","DOIUrl":"https://doi.org/10.1093/mnrasl/slad119","url":null,"abstract":"Gravitational waves (GWs) from binary black hole mergers provide unique opportunities for cosmological inference such as standard sirens. However, the accurate determination of the luminosity distance of the event is limited by the correlation between the distance and the angle between the binary's orbital angular momentum and the observer's line of sight. In the letter, we investigate the effect of precession on the distance estimation of binary black hole events for the third-generation (3G) GW detectors. We find that the precession can enhance the precision of distance inference by one order of magnitude compared to the scenario where precession is absent. The constraint on the host galaxies can be improved due to the improved distance measurement, therefore the Hubble constant can be measured with higher precision and accuracy. These findings underscore the noteworthy impact of precession on the precision of distance estimation for 3G ground-based GW detectors, which can serve as highly accurate probes of the Universe.","PeriodicalId":18951,"journal":{"name":"Monthly Notices of the Royal Astronomical Society: Letters","volume":"26 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135451910","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}
Previous studies of the massive nearby galaxy cluster Abell 3558 reported a cold front around the cluster core, which is attributed to the sloshing of the core as it responds to the gravitational disturbance created by a past minor merger. Here, using XMM-Newton mosaic, we report the detection of two rare large-scale sloshing cold fronts far outside the cooling radius of Abell 3558. One of the detected cold fronts is located 600 kpc from the cluster core to the south-east, while the other is located 1.2 Mpc from the cluster core to the north-west. The latter cold front is one of the most distant cold fronts ever observed in a galaxy cluster. Our findings are in agreement with previous studies that sloshing can extend well beyond the cooling radius, on scales exceeding half the virial radius, suggesting that sloshing is a cluster-wide phenomenon and may affect the cluster’s global properties.
{"title":"Two large-scale sloshing cold fronts in the outskirts of the galaxy cluster Abell 3558","authors":"M. Mirakhor, S. Walker, M. Sundquist, D. Chandra","doi":"10.1093/mnrasl/slad129","DOIUrl":"https://doi.org/10.1093/mnrasl/slad129","url":null,"abstract":"\u0000 Previous studies of the massive nearby galaxy cluster Abell 3558 reported a cold front around the cluster core, which is attributed to the sloshing of the core as it responds to the gravitational disturbance created by a past minor merger. Here, using XMM-Newton mosaic, we report the detection of two rare large-scale sloshing cold fronts far outside the cooling radius of Abell 3558. One of the detected cold fronts is located 600 kpc from the cluster core to the south-east, while the other is located 1.2 Mpc from the cluster core to the north-west. The latter cold front is one of the most distant cold fronts ever observed in a galaxy cluster. Our findings are in agreement with previous studies that sloshing can extend well beyond the cooling radius, on scales exceeding half the virial radius, suggesting that sloshing is a cluster-wide phenomenon and may affect the cluster’s global properties.","PeriodicalId":18951,"journal":{"name":"Monthly Notices of the Royal Astronomical Society: Letters","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-08-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"82355639","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}
M. Klinger, A. M. Taylor, T. Parsotan, A. Beardmore, S. Heinz, Sylvia J Zhu
We present counts-level fits to the multi-instrument (keV–GeV) data of the early afterglow (4 ks, 22 ks) of the brightest gamma-ray burst detected to date, GRB 221009A. The complexity of the data reduction, due to the unprecedented brightness and the location in the Galactic plane, is critically addressed. The energy spectrum is found to be well described by a smoothly broken power law with a break energy at a few keV. Three interpretations (slow/fast cooling or the transition between these) within the framework of forward shock synchrotron emission, from accelerated and subsequently cooled electrons, are found. The physical implications for each of these scenarios are discussed.
{"title":"The Multiwavelength Picture of GRB 221009A’s Afterglow","authors":"M. Klinger, A. M. Taylor, T. Parsotan, A. Beardmore, S. Heinz, Sylvia J Zhu","doi":"10.1093/mnrasl/slad185","DOIUrl":"https://doi.org/10.1093/mnrasl/slad185","url":null,"abstract":"We present counts-level fits to the multi-instrument (keV–GeV) data of the early afterglow (4 ks, 22 ks) of the brightest gamma-ray burst detected to date, GRB 221009A. The complexity of the data reduction, due to the unprecedented brightness and the location in the Galactic plane, is critically addressed. The energy spectrum is found to be well described by a smoothly broken power law with a break energy at a few keV. Three interpretations (slow/fast cooling or the transition between these) within the framework of forward shock synchrotron emission, from accelerated and subsequently cooled electrons, are found. The physical implications for each of these scenarios are discussed.","PeriodicalId":18951,"journal":{"name":"Monthly Notices of the Royal Astronomical Society: Letters","volume":"185 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2023-08-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139348921","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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