Astronomy & Astrophysics最新文献

{"title":"Charge sign dependence of recurrent Forbush decreases in 2016-2017","authors":"L. Romaneehsen, B. Heber, J. Marquardt","doi":"10.1051/0004-6361/202449836","DOIUrl":"https://doi.org/10.1051/0004-6361/202449836","url":null,"abstract":"This study investigates the periodicities of galactic cosmic ray flux attributed to CIR using Alpha Magnetic Spectrometer (AMS-02) data from late 2016 to early 2017. We determine the rigidity dependence of recurrent Forbush decrease (RFD) amplitudes induced by CIRs for different particles with a focus on charge sign. We carried out a frequency analysis using a Lomb-Scargle algorithm and superposed epoch analysis for all particles. For protons and helium, we compared the results with a single Forbush decrease (FD) analysis. Our results reveal that the rigidity dependence of proton amplitudes attributed to the northern coronal hole is in qualitative agreement with previous findings. In contrast, the amplitudes attributed to the southern coronal hole show no rigidity dependence. Furthermore, the amplitude of the helium modulation exceeds that of protons, in line with the observation for long-term modulation. For positrons, statistical limitations stand in the way of any definitive conclusions. In comparison to the positively charged particles, the modulation behavior of electrons reveals a different pattern.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":" 48","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141677886","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Exploring the connection between AGN radiative feedback and massive black hole spin","authors":"F. Bollati, A. Lupi, M. Dotti, F. Haardt","doi":"10.1051/0004-6361/202348538","DOIUrl":"https://doi.org/10.1051/0004-6361/202348538","url":null,"abstract":"We present a novel implementation for active galactic nucleus (AGN) feedback \u0000through ultrafast winds in the code gizmo . Our feedback recipe accounts for the angular dependence of radiative feedback on black hole spin. \u0000We self-consistently evolve in time (i) the gas-accretion process from resolved scales to a smaller scale unresolved (subgrid) AGN disk, (ii) the evolution of the spin of the massive black hole (MBH), (iii) the injection of AGN-driven winds into the resolved scales, and (iv) the spin-induced anisotropy of the overall feedback process. We tested our implementation by following the\u0000propagation of the wind-driven outflow into an homogeneous\u0000medium, and here we present a comparison of the results against simple analytical\u0000models. We also considered an isolated galaxy setup, where the galaxy is thought\u0000to be formed from the collapse of a spinning gaseous halo, and\u0000there we studied the impact of the AGN feedback on the evolution of the MBH and\u0000of the host galaxy. \u0000We find that: (i) AGN feedback limits the gas inflow that powers the MBH, with a consequent weak impact on the host galaxy characterized by a suppression of star\u0000formation by about a factor of two in the nuclear (lesssim kpc) region; (ii) the impact of AGN feedback on the host galaxy and on\u0000MBH growth is primarily determined by the AGN luminosity rather than by its angular pattern set by the MBH spin (i.e., more luminous AGNs more efficiently suppress central star formation (SF), clearing wider central cavities and driving outflows with larger semiopening angles);\u0000(iii) the imprint of the angular pattern of AGN radiation emission is detected more clearly at high (i.e., Eddington) accretion rates. At such high rates, the more isotropic angular patterns, as occur for high spin values, sweep away gas\u0000in the nuclear region more easily, therefore causing a slower MBH mass and spin growths and a higher quenching of SF.\u0000We argue that the influence of spin-dependent anisotropy of AGN feedback on MBH and galaxy evolution is likely to be relevant in those scenarios characterized by high and prolonged MBH accretion episodes and by high AGN wind--galaxy coupling. Such conditions are more frequently met in galaxy mergers and/or high-redshift galaxies.","PeriodicalId":505693,"journal":{"name":"Astronomy & Astrophysics","volume":" 11","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141678104","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"SRG/eROSITA 3D mapping of the interstellar medium using X-ray absorption spectroscopy","authors":"E. Gatuzz, J. Wilms, A. Zainab, S. Freund, P. Schneider, J. Robrade, S. Czesla, J. A. García, T. Kallman","doi":"10.1051/0004-6361/202449374","DOIUrl":"https://doi.org/10.1051/0004-6361/202449374","url":null,"abstract":"We present a detailed study of the hydrogen density distribution in the local interstellar medium (ISM) using the X-ray absorption technique.\u0000Hydrogen column densities were precisely measured by fitting X-ray spectra from coronal sources observed during the initial eROSITA all-sky survey (eRASS1).\u0000Accurate distance measurements were obtained through cross-matching Galactic sources with the third Gaia data release (DR3).\u0000Despite the absence of a discernible correlation between column densities and distances or Galactic longitude, a robust correlation with Galactic latitude was identified. \u0000This suggests a decrease in ISM material density in the vertical direction away from the Galactic plane. \u0000We have also investigated the relation between the optical extinction and the hydrogen column density.\u0000To do so, we employed multiple density laws to fit the measured column densities, revealing constraints on height scale values ($9 < h_ z < 14$ pc). \u0000Unfortunately, radial scales and the central density remain unconstrained due to the scarcity of sources near the Galactic center. \u0000Subsequently, a 3D density map of the ISM was computed using a Gaussian process approach, inferring hydrogen density distribution from hydrogen column densities. \u0000The results unveil the presence of multiple beams and clouds of various sizes, indicative of small-scale structures. \u0000High-density regions were identified at approximately 100 pc, consistent with findings in dust-reddening studies, and are potentially associated with the Galactic Perseus arm or the local bubble.\u0000Moreover, high-density regions were pinpointed in proximity to the Orion, Chameleon, and Coalsack molecular complex, enriching our understanding of the intricate structure of the local ISM.","PeriodicalId":505693,"journal":{"name":"Astronomy &amp; Astrophysics","volume":" 33","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141677980","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Testing a non-local 1-equation turbulent convection model: A solar model","authors":"T. A. M. Braun, F. Ahlborn, A. W. M. F. Astrophysik, Garching, Germany, Ludwig-Maximilians-Universitat Munchen, Munich, Heidelberger Institut fur Theoretische Studien, Heidelberg","doi":"10.1051/0004-6361/202450511","DOIUrl":"https://doi.org/10.1051/0004-6361/202450511","url":null,"abstract":"Turbulent convection models treat stellar convection more physically than standard mixing-length theory by including non-local effects. We recently successfully applied the Kuhfuss version to convective cores in main sequence stars. Its usefulness for convective envelopes remains to be tested. The solar convective envelope constitutes a viable test bed for investigating the usefulness of the 1-equation Kuhfuss turbulent convection model. We used the one-dimensional stellar evolution code GARSTEC to calculate a standard solar model with the 1-equation Kuhfuss turbulent convection model, and compared it to helioseismic measurements and a solar model using standard mixing-length theory. Additionally, we investigated the influence of the additional free parameters of the convection model on the solar structure. The 1-equation Kuhfuss model reproduces the sound-speed profile and the lower boundary of the convective region less well than the mixing-length model, because the inherent non-local effects overestimate the amount of convective penetration below the Schwarzschild boundary. We trace this back to the coupling of the temperature gradient to the convective flux in the 1-equation version of the Kuhfuss theory. The temperature stratification of the solar convective envelope is not well modelled by the 1-equation Kuhfuss turbulent convection model, and the more complex 3-equation version is needed to improve the modelling of convection in the envelopes of 1D stellar evolution models.","PeriodicalId":505693,"journal":{"name":"Astronomy &amp; Astrophysics","volume":" 7","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141678506","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Progenitor mass and ejecta asymmetry of supernova 2023ixf from nebular spectroscopy","authors":"L. Ferrari, G. Folatelli, K. Ertini, H. Kuncarayakti, Jennifer E. Andrews","doi":"10.1051/0004-6361/202450440","DOIUrl":"https://doi.org/10.1051/0004-6361/202450440","url":null,"abstract":"Supernova (SN) 2023ixf was discovered in the galaxy M101 in May 2023. Its proximity provided the scientific community an extremely valuable opportunity to study the characteristics of the SN and its progenitor. \u0000 A point source detected on archival images and hydrodynamical modeling of the bolometric light curve have been used to constrain the former star's properties. \u0000 There is a significant variation in the published results regarding the initial mass of the progenitor.\u0000 Nebular spectroscopy can be used to enhance our understanding of the SN and its progenitor. We determined the SN progenitor mass by studying the first published nebular spectrum, taken 259 days after the explosion. We analyzed the nebular spectrum taken with GMOS at the Gemini North Telescope. We identified typical emission lines, such as O i Halpha , and Ca ii among others. Some species' line profiles show broad and narrow components, indicating two ejecta velocities and an asymmetric ejecta. We inferred the progenitor mass of SN 2023ixf by comparing its spectra with synthetic spectra and by measuring the forbidden oxygen doublet flux. Based on the flux ratio and the direct comparison with spectra models, the progenitor star of SN 2023ixf had a $M_ ZAMS $ between 12 and 15 $M_ We find that using the O i doublet flux provides a less tight constraint on the progenitor mass.\u0000 Our results agree with those from hydrodynamical modeling of the early light curve and pre-explosion image estimates that point to a relatively low-mass progenitor.","PeriodicalId":505693,"journal":{"name":"Astronomy &amp; Astrophysics","volume":" 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141678295","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Measuring stellar surface rotation and activity with the PLATO mission. I. Strategy and application to simulated light curves","authors":"S. Breton, A. Lanza, S. Messina, I. Pagano, L. Bugnet, E. Corsaro, R. Garc'ia, S. Mathur, A.R.G. Santos, S. Aigrain, L. Amard, A. S. Brun, L. Degott, Q. Noraz, D. B. Palakkatharappil, E. Panetier, A. Strugarek, K. Belkacem, M. Goupil, R. Ouazzani, J. Philidet, C. Renié, O. Roth","doi":"10.1051/0004-6361/202449893","DOIUrl":"https://doi.org/10.1051/0004-6361/202449893","url":null,"abstract":"The Planetary Transits and Oscillations of stars mission (PLATO) will allow us to measure surface rotation and monitor photometric activity of tens of thousands of main sequence solar-type and subgiant stars.\u0000 \u0000 This paper is the first of a series dedicated to the preparation of the analysis of stellar surface rotation and photospheric activity with the near-future PLATO data.\u0000 We describe in this work the strategy that will be implemented in the PLATO pipeline to measure stellar surface rotation, photometric activity, and long-term modulations.\u0000 \u0000 The algorithms are applied on both noise-free and noisy simulations of solar-type stars, which include activity cycles, latitudinal differential rotation, and spot evolution. PLATO simulated systematics are included in the noisy light curves.\u0000 \u0000 We show that surface rotation periods can be recovered with confidence for most of the stars with only six months of observations and that the recovery rate of the analysis significantly improves as additional observations are collected. This means that the first PLATO data release will already provide a substantial set of measurements for this quantity, with a significant refinement on their quality as the instrument obtains longer light curves. \u0000 \u0000 Measuring the Schwabe-like magnetic activity cycle during the mission will require that the same field be observed over a significant timescale (more than four years). Nevertheless, PLATO will provide a vast and robust sample of solar-type stars with constraints on the activity-cycle length. Such a sample is lacking from previous missions dedicated to space photometry.","PeriodicalId":505693,"journal":{"name":"Astronomy &amp; Astrophysics","volume":" 14","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141678164","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The story of SN 2021aatd: A peculiar 1987A-like supernova with an early-phase luminosity excess","authors":"T. Szalai, R. Könyves-Tóth, A. P. Nagy, D. Hiramatsu, I. Arcavi, A. Bostroem, D. A. Howell, J. Farah, C. McCully, M. Newsome, E. Padilla Gonzalez, C. Pellegrino, G. Terreran, E. Berger, P. Blanchard, S. Gomez, P. Székely, D. Banhidi, I.B. Bíró, I. Csányi, A. Pál, J. Rho, J. Vinko","doi":"10.1051/0004-6361/202348548","DOIUrl":"https://doi.org/10.1051/0004-6361/202348548","url":null,"abstract":"There is a growing number of peculiar events that cannot be assigned to any of the main classes. SN 1987A and a handful of similar objects, thought to be explosive outcomes of blue supergiant stars, is one of them: while their spectra closely resemble those of H-rich (IIP) SNe, their light curve (LC) evolution is very different. Here we present the detailed photometric and spectroscopic analysis of SN 2021aatd, a peculiar Type II explosion. While its early-time evolution resembles that of the slowly evolving double-peaked SN 2020faa (although at a lower luminosity scale), after sim 40 days its LC shape becomes similar to that of SN 1987A-like explosions. In addition to comparing LCs, color curves, and spectra of SN 2021aatd to those of SNe 2020faa, 1987A, and other objects, we compared the observed spectra with our own SYN++ models and with the outputs of published radiative transfer models. We also carried out a detailed modeling of the pseudo-bolometric LCs of SNe 2021aatd and 1987A with a self-developed semi-analytical code, assuming a two-component ejecta (core + shell), and involving the rotational energy of a newborn magnetar in addition to radioactive decay. We find that the photometric and the spectroscopic evolution of SN 2021aatd can be well described with the explosion of a sim 15 $M_ blue supergiant star. Nevertheless, SN 2021aatd shows higher temperatures and weaker Na i D and Ba ii lines than SN 1987A, which is instead reminiscent of IIP-like atmospheres. With the applied two-component ejecta model (accounting for decay and magnetar energy), we can successfully describe the bolometric LC of SN 2021aatd, including the first sim 40-day phase showing an excess compared to 87A-like SNe, but being strikingly similar to that of the long-lived SN 2020faa. Nevertheless, finding a unified model that also explains the LCs of more luminous events (e.g., SN 2020faa) is still a matter of debate.","PeriodicalId":505693,"journal":{"name":"Astronomy &amp; Astrophysics","volume":" 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141677906","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Unexpected frequency of horizontal oscillations of magnetic structures in the solar photosphere","authors":"M. Berretti, M. Stangalini, G. Verth, S. Jafarzadeh, D. Jess, F. Berrilli, S. Grant, T. Duckenfield, V. Fedun","doi":"10.1051/0004-6361/202450693","DOIUrl":"https://doi.org/10.1051/0004-6361/202450693","url":null,"abstract":"It is well known that the dominant frequency of oscillations in the solar photosphere is approx 3 mHz, which is the result of global resonant modes pertaining to the whole stellar structure. However, analyses of the horizontal motions of nearly $1$ million photospheric magnetic elements spanning the entirety of solar cycle 24 have revealed an unexpected dominant frequency, approx 5 mHz, a frequency typically synonymous with the chromosphere. Given the distinctly different physical properties of the magnetic elements examined in our statistical sample, when compared to largely quiescent solar plasma where approx 3 mHz frequencies are omnipresent, we argue that the dominant approx 5 mHz frequency is not caused by the buffeting of magnetic elements, but instead is due to the nature of the underlying oscillatory driver itself. This novel result was obtained by exploiting the unmatched spatial and temporal coverage of magnetograms acquired by the Helioseismic and Magnetic Imager (HMI) on board NASA's Solar Dynamics Observatory (SDO). Our findings provide a timely avenue for future exploration of the magnetic connectivity between sub-photospheric, photospheric, and chromospheric layers of the Sun's dynamic atmosphere.","PeriodicalId":505693,"journal":{"name":"Astronomy &amp; Astrophysics","volume":" 38","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141679328","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Fast supermassive black hole growth in the SPT2349--56 protocluster at z=4.3","authors":"F. Vito, W. N. Brandt, A. Comastri, R. Gilli, J.R. Ivison, G. Lanzuisi, B. Lehmer, I. E. Lopez, P. Tozzi, C. Vignali","doi":"10.1051/0004-6361/202450225","DOIUrl":"https://doi.org/10.1051/0004-6361/202450225","url":null,"abstract":"Large-scale environment is one of the main physical drivers of galaxy evolution. The densest regions at high redshifts (i.e. $z>2$ protoclusters) are gas-rich regions characterised by high star formation activity. The same physical properties that enhance star formation in protoclusters are also thought to boost the growth of supermassive black holes (SMBHs), most likely in heavily obscured conditions. We aim to test this scenario by probing the active galactic nucleus (AGN) content of SPT2349--56: a massive, gas-rich, and highly star-forming protocluster core at $z=4.3$ discovered as an overdensity of dusty star-forming galaxies (DSFGs). We compare our results with data on the field environment and other protoclusters We observed SPT2349--56 with Chandra (200 ks) and searched for X-ray emission from the known galaxy members. We also performed a spectral energy distribution fitting procedure to derive the physical properties of the discovered AGNs. In the X-ray band, we detected two protocluster members: C1 and C6, corresponding to an AGN fraction among DSFGs in the structure of $ This value is consistent with other protoclusters at $z=2-4$, but higher than the AGN incidence among DSFGs in the field environment. Both AGNs are heavily obscured sources, hosted in star-forming galaxies with $ M_ odot $ stellar masses. We estimate that the intergalactic medium in the host galaxies contributes to a significant fraction (or even entirely) to the nuclear obscuration. In particular, C1 is a highly luminous ($L_X=2 and Compton-thick ($N_H=2 cm^ $) AGN, likely powered by a $M_ BH M_ odot $ SMBH, assuming Eddington-limited accretion. Its high accretion rate suggests that it is in the phase of efficient growth that is generally required to explain the presence of extremely massive SMBHs in the centres of local galaxy clusters. Considering SPT2349--56 and DRC, a similar protocuster at $z=4$, and under different assumptions on their volumes, we find that gas-rich protocluster cores at $z enhance the triggering of luminous (log$ L_X lunit =45-46$) AGNs by three to five orders of magnitude with respect to the predictions from the AGN X-ray luminosity function at a similar redshift in the field environment. We note that this result is not solely driven by the overdensity of the galaxy population in the structures. Our results indicate that gas-rich protoclusters at high redshift boost the growth of SMBHs, which will likely impact the subsequent evolution of the structures. Therefore, they stand as key science targets to obtain a complete understanding of the relation between the environment and galaxy evolution. Dedicated investigations of similar protoclusters are required to definitively confirm this conclusion with a higher statistical significance.","PeriodicalId":505693,"journal":{"name":"Astronomy &amp; Astrophysics","volume":" 26","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141680812","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"NOEMA formIng Cluster survEy (NICE): Characterizing eight massive galaxy groups at 1.5< z<4 in the COSMOS field","authors":"N. Sillassen, S. Jin, G. Magdis, E. Daddi, Tao Wang, Shiying Lu, Hanwen Sun, V. Arumugam, Daizhong Liu, M. Brinch, C. D’Eugenio, R. Gobat, C. G'omez-Guijarro, M. Rich, E. Schinnerer, V. Strazzullo, Qing-Hua Tan, F. Valentino, Yijun Wang, M. Xiao, Luwenjia Zhou, David Bl'anquez-Ses'e, Zheng Cai, Yanmei Chen, L. Ciesla, Yu Dai, I. Delvecchio, David Elbaz, A. Finoguenov, F. Gao, Qiusheng Gu, Catherine Hale, Q. Hao, Jiasheng Huang, Matt J. Jarvis, B. Kalita, Xu Ke, A. L. Bail, B. Magnelli, Yong Shi, Mattia Vaccari, I. Whittam, Tiancheng Yang, Zhi-Yun Zhang","doi":"10.1051/0004-6361/202450760","DOIUrl":"https://doi.org/10.1051/0004-6361/202450760","url":null,"abstract":"The NOrthern Extended Millimeter Array (NOEMA) formIng Cluster survEy (NICE) is a NOEMA large programme targeting 69 massive galaxy group candidates at $z>2$ over six deep fields with a total area of 46 deg$^2$. Here we report the spectroscopic confirmation of eight massive galaxy groups at redshifts $1.65 z in the Cosmic Evolution Survey (COSMOS) field. Homogeneously selected as significant overdensities of red IRAC sources that have red Herschel colours, four groups in this sample are confirmed by CO and CI line detections of multiple sources with NOEMA 3mm observations, three are confirmed with Atacama Large Millimeter Array (ALMA) observations, and one is confirmed by Halpha emission from Subaru/FMOS spectroscopy. \u0000Using rich ancillary data in the far-infrared and sub-millimetre, we constructed the integrated far-infrared spectral energy distributions for the eight groups, obtaining a total infrared star formation rate (SFR) of 260-1300 $ M_ odot $ yr$^ $.\u0000We adopted six methods for estimating the dark matter masses of the eight groups, including stellar mass to halo mass relations, overdensity with galaxy bias, and NFW profile fitting to radial stellar mass densities. We find that the radial stellar mass densities of the eight groups are consistent with a NFW profile, supporting the idea that they are collapsed structures hosted by a single dark matter halo. The best halo mass estimates are $ h M_ odot )=12.8-13.7$ with a general uncertainty of 0.3 dex.\u0000Based on the halo mass estimates, we derived baryonic accretion rates (BARs) of $(1-8) odot /yr $ for this sample. Together with massive groups in the literature, we find a quasi-linear correlation between the integrated SFR/BAR ratio and the theoretical halo mass limit for cold streams, $M_ stream /M_ h $, with $ SFR/BAR pm0.22 M_ stream /M_ h pm0.16 dex $.\u0000Furthermore, we compared the halo masses and the stellar masses with simulations, and find that the halo masses of all structures are consistent with those of progenitors of $M_ h (z=0)>10^ odot $ galaxy clusters, and that the most massive central galaxies have stellar masses consistent with those of the brightest cluster galaxy progenitors in the TNG300 simulation. Above all, the results strongly suggest that these massive structures are in the process of forming massive galaxy clusters via baryonic and dark matter accretion.","PeriodicalId":505693,"journal":{"name":"Astronomy &amp; Astrophysics","volume":"104 7","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-07-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141683613","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}