Star clusters near and far; tracing star formation across cosmic time
Angela Adamo, Peter Zeidler, J. M. Diederik Kruijssen, Mélanie Chevance, Mark Gieles, Daniela Calzetti, Corinne Charbonnel, Hans Zinnecker, Martin G. H. Krause
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Final published version. 61 pages, 10 figures. To appear in Space Science Reviews (submitted January 31, 2020; accepted May 8, 2020), topical collection Star formation
Star clusters are fundamental units of stellar feedback and unique tracers of their host galactic properties. In this review, we will first focus on their constituents, i.e.\ detailed insight into their stellar populations and their surrounding ionised, warm, neutral, and molecular gas. We, then, move beyond the Local Group to review star cluster populations at various evolutionary stages, and in diverse galactic environmental conditions accessible in the local Universe. At high redshift, where conditions for cluster formation and evolution are more extreme, we are only able to observe the integrated light of a handful of objects that we believe will become globular clusters. We therefore discuss how numerical and analytical methods, informed by the observed properties of cluster populations in the local Universe, are used to develop sophisticated simulations potentially capable of disentangling the genetic map of galaxy formation and assembly that is carried by globular cluster populations.
The rate of ionization by cosmic rays in interstellar gas directly associated with gamma-ray emitting supernova remnants is for the first time calculated to be several orders of magnitude larger than the Galactic average. Analysis of ionization-induced chemistry yields the first quantitative prediction of the astrophysical H_{2}^{+} emission line spectrum, which should be detectable together with H_3^+ lines. The predicted coincident observation of those emission lines and gamma-rays will help prove that supernova remnants are sources of cosmic rays.
Dwarf galaxies are thought to quench primarily due to environmental processes most typically occurring in galaxy groups and clusters or around single, massive galaxies. However, at earlier epochs, ($5 < z < 2$), the collapse of large scale structure (forming Zel'dovich sheets and subsequently filaments of the cosmic web) can produce volume-filling accretion shocks which elevate large swaths of the intergalactic medium (IGM) in these structures to a hot ($T>10^6$ K) phase. We study the impact of such an event on the evolution of central dwarf galaxies ($5.5 < \log M_* < 8.5$) in the field using…
We report on the effects of cosmic rays (CRs) on the abundance of CO in $\rm H_2$ clouds under conditions typical for star-forming galaxies in the Universe. We discover that this most important molecule for tracing H$_2$ gas is very effectively destroyed in ISM environments with CR energy densities $\rm U_{CR}\sim(50-10^{3})\times U_{CR,Gal}$, a range expected in numerous star-forming systems throughout the Universe. This density-dependent effect operates volumetrically rather than only on molecular cloud surfaces (i.e. unlike FUV radiation that also destroys CO), and is facilitated by: a) the…
Connecting galaxies with their descendants (or progenitors) at different redshifts can yield strong constraints on galaxy evolution. Observational studies have historically selected samples of galaxies using a physical quantity, such as stellar mass, either above a constant limit or at a constant cumulative number density. Investigation into the efficacy of these selection methods has not been fully explored. Using a set of four semi-analytical models based on the output of the Millennium Simulation, we find that selecting galaxies at a constant number density (in the range $-4.3 < \log\ n\ [\…
Tracing cosmic star formation history through radio continuum spectral energy distribution and non-thermal emission
Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Institute for Research in Fundamental Sciences (IPM)（伊朗基础科学研究所）；University of Cologne（科隆大学）；International Centre for Radio Astronomy Research, Curtin University（西澳大学国际射电天文研究中心）；Hunan Normal University（湖南师范大学）；Nanjing University（南京大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Academia Sinica（中央研究院）；University of Hertfordshire（赫特福德大学）；University of the Western Cape（西开普大学）
We propose a method of searching for radio sources exhibiting the Sunyaev-Zeldovich effect in the multi-frequency emission maps from the Planck mission data using a convolutional neural network. A catalog for recognizing radio sources is compiled using the GLESP pixelation scheme at the frequencies of 100, 143, 217, 353, and 545 GHz. The quality of the proposed approach is evaluated and the quality of the dependence of model data on the S/N ratio is estimated. We show that the presented neural network approach allows the detection of sources with the Sunyaev-Zeldovich effect. The proposed meth…
Tracing Cold Gas in Absorption Across Cosmic Time with the SKA
Inter-University Centre for Astronomy and Astrophysics（天文与天体物理跨大学中心）；Ioffe Institute（约费研究所）；Indian Institute of Astrophysics (IIA)（印度天体物理研究所）；Centre for Astrophysics and Supercomputing, Swinburne University of Technology（天体物理学与超级计算中心，斯威本科技大学）；French-Chilean Laboratory for Astronomy, IRL 3386, CNRS and Universidad de Chile（法智利天体物理实验室，IRL 3386，法国国家科学研究中心和智利大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Wits Centre for Astrophysics, School of Physics, University of the Witwatersrand（维特沃特斯兰德大学物理学院天体物理中心）；Institut d'Astrophysique de Paris, CNRS（巴黎天体物理研究所，法国国家科学研究中心）；Pole Scientific, University Catholic of Lyon（里昂天主教大学科学学部）；Sydney Institute for Astronomy, School of Physics A28, University of Sydney（悉尼大学物理学院A28天文研究所）；Astronomy Department, National Research Institute of Astronomy and Geophysics (NRIAG)（天体物理与地球物理国家研究所天文系）；International Centre for Radio Astronomy Research, Curtin University（科廷大学国际射电天文研究中心）；Korea Astronomy and Space Science Institute（韩国天文学与空间科学研究院）
Gravitational Waves from Cosmic Dawn: Tracing Cosmic Black Hole Binaries with ET, LGWA, and LISA
INAF/Osservatorio Astronomico di Roma（罗马天文台）；INFN, Sezione Roma1（罗马第一分部意大利国家核物理研究所）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Sapienza School for Advanced Studies（萨皮恩扎高等研究学院）
With the installation of the Cosmic Origins Spectrograph on the Hubble Space Telescope, measurements of the metal content of the low redshift intergalactic medium (IGM) are now available. Using a new grid-based model for diffuse gas coupled to the SAGE semi-analytic model of galaxy formation, we examine the impact of supernova feedback on the pollution of the IGM. We consider different assumptions for the reheating and ejection of gas by supernovae and their dependence on galaxy circular velocity and gas surface density. Where metals are present, we find the most likely metallicity to be $-1.5…
SAMI and TNG-Cluster: tracing galaxy spin and environmental transformation across cluster phase-space and cosmic time
Universidade Tecnológica Federal do Paraná（帕拉纳联邦技术大学）；European Southern Observatory（欧洲南方天文台）；Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo（圣保罗大学天文、地球物理与大气科学研究所）；University of Dodoma, College of Natural and Mathematical Sciences（多多马大学自然与数理科学学院）
Roman CCS White Paper: Tracing stellar mass assembly and emerging quiescence at cosmic noon -- the case for deep imaging with all of Roman's wide filters in the HLTDS
本文论证了在 Roman 望远镜 HLTDS 中使用除 F146 外所有宽滤光片进行深度成像的必要性，以推动河外深场科学并改进 SN Ia 宇宙学系统学。
Tracing the Cosmic web across Cosmic time through SKA observations of radio galaxies
National Centre for Nuclear Research（国家核研究中心）；University of Tartu（塔尔图大学）；Assam Don Bosco University（阿萨姆唐博斯科大学）；Observatoire de Paris（巴黎天文台）；Collège de France（法兰西公学院）；PSL University（PSL大学）；Sorbonne University（索邦大学）
At present, all physical models of diffuse Galactic gamma-ray emission assume that the distribution of cosmic-ray sources traces the observed populations of either OB stars, pulsars, or supernova remnants. However, since H2-rich regions host significant star formation and numerous supernova remnants, the morphology of observed H2 gas should also provide a physically motivated, high-resolution tracer for cosmic-ray injection. We assess the impact of utilizing H2 as a tracer for cosmic-ray injection on models of diffuse Galactic gamma-ray emission. We employ state-of-the-art 3D particle diffusio…
Despite their ubiquity, the origin of cosmic magnetic fields remains unknown. Various mechanisms have been proposed for their existence including primordial fields generated by inflation, or amplification and injection by compact astrophysical objects. Separating the potential impact of each magnetogenesis scenario on the magnitude and orientation of the magnetic field and their impact on gas dynamics may give insight into the physics that magnetised our Universe. In this work, we demonstrate that because the induction equation and solenoidal constraint are linear with $B$, the contribution fr…
We study the mass assembly and spin evolution of supermassive black holes (BHs) across cosmic time as well as the impact of gravitational recoil on the population of nuclear and wandering black holes (wBHs) by using the semi-analytical model LGalaxies run on top of Millennium merger trees. We track spin changes that BHs experience during both coalescence events and gas accretion phases. For the latter, we assume that spin changes are coupled with the bulge assembly. This assumption leads to predictions for the median spin values of z=0 BHs that depend on whether they are hosted by pseudobulges…
We trace the cosmic web at redshifts 1.0 <= z <= 1.8 using the quasar data from the SDSS DR7 QSO catalogue (Schneider et al. 2010). We apply a friend-of-friend (FoF) algorithm to the quasar and random catalogues to determine systems at a series of linking lengths, and analyse richness and sizes of these systems. At the linking lengths l <= 30 Mpc/h the number of quasar systems is larger than the number of systems detected in random catalogues, and systems themselves have smaller diameters than random systems. The diameters of quasar systems are comparable to the sizes of poor galaxy superclust…
We study a sample of Herschel-PACS selected galaxies within the GOODS-South and the COSMOS fields in the framework of the PACS Evolutionary Probe (PEP) project. Starting from the rich multi-wavelength photometric data-sets available in both fields, we perform a broad-band Spectral Energy Distribution (SED) decomposition to disentangle the possible active galactic nucleus (AGN) contribution from that related to the host galaxy. We find that 37 per cent of the Herschel-selected sample shows signatures of nuclear activity at the 99 per cent confidence level. The probability to reveal AGN activity…
Tracing small-scale structure formation through cosmic time with strong gravitational lensing: A case for a next-generation sub-millimetre/millimetre interferometer
European Southern Observatory (ESO)（欧洲南方天文台）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；South African Radio Astronomy Observatory (SARAO)（南非射电天文观测台）；Department of Physics, University of Pretoria（比勒陀利亚大学物理系）；Pole Scientific, Catholic University of Lyon（里昂天主教大学科学部门）；Instituto de Física y Astronomía, Universidad de Valparaíso（瓦尔帕莱索大学物理与天文学研究所）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；Department of Physics, University of Oxford（牛津大学物理系）；Observatoire de Paris, LUX, Collège de France, CNRS, PSL University, Sorbonne University（巴黎天文台，卢克斯，法兰西公学院，法国国家科学研究中心，巴黎文理研究大学，索邦大学）；Dipartimento di Fisica e Astronomia Augusto Righi , Università di Bologna（博洛尼大学奥古斯托·里吉物理与天文学系）；INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚空间科学与天文学观测台）；INFN – Sezione di Bologna（意大利国家核物理研究所博洛尼亚分部）
The intrinsic alignment of galaxies is an important systematic effect in weak-lensing surveys, which can affect the derived cosmological parameters. One direct way to distinguish different alignment models and quantify their effects on the measurement is to produce mocked weak-lensing surveys. In this work, we use full-sky ray-tracing technique to produce mock images of galaxies from the ELUCID $N$-body simulation run with the WMAP9 cosmology. In our model we assume that the shape of central elliptical galaxy follows that of the dark matter halo, and spiral galaxy follows the halo spin. Using …
Tracing Radio AGN-Driven Quenching in Post-Starburst Galaxies at Cosmic Noon
Johns Hopkins University（约翰斯·霍普金斯大学）；Space Telescope Science Institute（太空望远镜科学研究所）；AURA for ESA, Space Telescope Science Institute（欧洲空间局阿雷西博大学协会太空望远镜科学研究所）；University of Nottingham（诺丁汉大学）；University of St Andrews（圣安德鲁斯大学）；University of Edinburgh（爱丁堡大学）；European Southern Observatory (ESO)（欧洲南方天文台）
Tracing the Cosmic Evolution of the Cool Circumgalactic Medium of Luminous Red Galaxies with DESI Year 1 Data
Graduate Institute of Astrophysics, National Taiwan University（台湾大学天文研究所）；Department of Physics, National Taiwan University（台湾大学物理系）；Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；Kavli Institute for the Physics and Mathematics of the Universe（宇宙物理数学卡弗里研究所）；Institute of Space Sciences, ICE-CSIC（空间科学研究所，西班牙国家科学研究委员会）；Instituto Astrofisica de Canarias（加那利群岛天体物理研究所）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Department of Physics, Boston University（波士顿大学物理系）；Dipartimento di Fisica “Aldo Pontremoli”, Università degli Studi di Milano（米兰大学阿尔多·蓬特罗利物理系）；INAF-Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）
We investigate the effects of primordial non-Gaussianities in the primordial Universe on the baryonic structure formation process. By relating the cosmic star formation rate in Gaussian and non-Gaussian scenarios to the detectability of high-redshift sources of reionization, we derive the expected Gamma-Ray Burst rate in the different models. We find that counts of high-redshift Gamma-Ray Bursts can be used as cosmological probes of non-Gaussianities and that they are suitable candidates to distinguish non-Gaussian effects at early epochs.
The $e$MERLIN Galaxy Evolution Survey ($e$MERGE) is an ambitious, multi-tiered extragalactic radio continuum survey being carried out with $e$MERLIN and the VLA at 1.4GHz and 6GHz. Exploiting the unique combination of high sensitivity and high angular resolution provided by radio interferometry, these observations will provide a powerful, obscuration-independent tool for tracing intense star-formation and AGN activity in galaxies out to $z\sim5$. In our first data release (DR1) we present $e$MERGE Tier 1, a 15-arcmin pointing centred on the GOODS-N field, imaged at 1.4GHz with the VLA and $e$M…
We present analysis on three intervening H I-C IV absorption systems tracing gas within galaxy group/cluster environments, identified in the $HST$/COS far-UV spectra of the background quasars PG $1148+549$ ($z_{abs}=0.00346$), SBS~$1122+594$ ($z_{abs}=0.00402$) and RXJ~$1230.8+0115$ ($z_{abs}=0.00574$). The ionization models are consistent with the origin of metal lines and H I from a cool and diffuse photoionized gas phase with $T \lesssim 4 \times 10^{4}$ K and $n_{\mathrm{H}} \lesssim 5 \times 10^{-4}$ cm$^{-3}$. The three absorbers have $89$, $51$ and $17$ galaxies detected within $1$ Mpc …
Tracing nitrogen enrichment across cosmic time with JWST
Università di Firenze（佛罗伦萨大学）；INAF – Arcetri Astrophysical Observatory（意大利国家天体物理研究所阿切特里天文台）；European Southern Observatory（欧洲南方天文台）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）
The cosmic origin of fluorine is still under debate. Asymptotic giant branch (AGB) stars are among the few suggested candidates to efficiently synthesis F in our Galaxy, however their relative contribution is not clear. In this paper, we briefly review the theoretical studies from stellar yield models of the F synthesis and chemical equilibrium models of the F-containing molecules in the outflow around AGB stars. Previous detections of the F-bearing species towards AGB and post-AGB stars are also highlighted. We suggest that high-resolution ALMA observations of the AlF, one of the two main car…
Using the Cosmic Origins Spectrograph aboard the Hubble Space Telescope, we measured the abundances of six ions (C III, C IV, Si III, Si IV, N V, O VI) in the low-redshift (z < 0.4) intergalactic medium and explored C and Si ionization corrections from adjacent ion stages. Both C IV and Si IV have increased in abundance by a factor of ~10 from z = 5.5 to the present. We derive ion mass densities, (rho_ion) = (Omega_ion)(rho_cr) with Omega_ion expressed relative to closure density. Our models of the mass-abundance ratios, (Si III / Si IV) = 0.67(+0.35,-0.19), (C III / C IV) = 0.70(+0.43,-0.20),…
We analyse the physical properties of 121 SNR $\geq$ 5 sub-millimetre galaxies (SMGs) from the STUDIES 450-$μ$m survey. We model their UV-to-radio spectral energy distributions using MAGPHYS+photo-$z$ and compare the results to similar modelling of 850-$μ$m-selected SMG sample from AS2UDS, to understand the fundamental physical differences between the two populations at the observed depths. The redshift distribution of the 450-$μ$m sample has a median of $z$ = 1.85 $\pm$ 0.12 and can be described by strong evolution of the far-infrared luminosity function. The fainter 450-$μ$m sample has $\sim…
Tracing Galaxy Bias Through the Cosmic Web: The Role of Filaments
Universidad Técnica Federico Santa María（弗雷德里克·Santa Maria 技术大学）；Pontificia Universidad Católica de Valparaíso（瓦爾帕萊索天主教大學）；The University of Tokyo（東京大學）；University of Pennsylvania（賓夕法尼亞大學）；The Abdus Salam International Center for Theoretical Physics（阿卜杜斯·薩拉姆國際理論物理中心）；Universidad Nacional de Córdoba（科爾多瓦國立大學）；CONICET-UNC（阿根廷國家科學技術研究委員會-科爾多瓦大學）
A key for understanding the evolution of galaxies and in particular their star formation history will be future ultra-deep radio surveys. While star formation rates (SFRs) are regularly estimated with phenomenological formulas based on the local FIR-radio correlation, we present here a physically motivated model to relate star formation with radio fluxes. Such a relation holds only in frequency ranges where the flux is dominated by synchrotron emission, as this radiation originates from cosmic rays produced in supernova remnants, therefore reflecting recent star formation. At low frequencies s…
We explore how the estimated star formation rate (SFR) of a sample of isolated, massive dusty star-forming galaxies at early cosmic epochs ($1.5 < z < 3.5$) changes when their ultraviolet (UV) to near-infrared (NIR) spectral energy distribution is extended to longer wavelengths by adding far-infrared/sub-millimeter data to trace the reprocessed radiation from dust heated by young massive stars. We use large-area surveys with multi-wavelength datasets that include DECam UV-to-optical, VICS82 NIR, Spitzer-IRAC NIR, and Herschel-SPIRE far-infrared/sub-millimeter data. We find that the inclusion o…
Cosmic far-infrared background (CFIRB) probes unresolved dusty star-forming galaxies across cosmic time and is complementary to ultraviolet and optical observations of galaxy evolution. In this work, we interpret the observed CFIRB anisotropies using an empirical model based on resolved galaxies in ultraviolet and optical surveys. Our model includes stellar mass functions, star-forming main sequence, and dust attenuation. We find that the commonly used linear Kennicutt relation between infrared luminosity and star formation rate overproduces the observed CFIRB amplitudes. The observed CFIRB re…
Cosmic far-infrared background (CFIRB) is a powerful probe of the history of star formation rate (SFR) and the connection between baryons and dark matter across cosmic time. In this work, we explore to which extent the CFIRB anisotropies can be reproduced by a simple physical framework for galaxy evolution, the gas regulator (bathtub) model. This model is based on continuity equations for gas, stars, and metals, taking into account cosmic gas accretion, star formation, and gas ejection. We model the large-scale galaxy bias and small-scale shot noise self-consistently, and we constrain our mode…
Galaxies are thought to reside inside of large gravitationally bound structures of dark matter, so-called haloes. While the smallest of these haloes host no or only a few stars, the biggest host entire clusters of galaxies. Over cosmic history, haloes often collided and merged, forming bigger and bigger structures. Merger trees, i.e., catalogues of haloes evolving and connections between them as they grow and merge, have become a vital tool in describing and understanding the history of cosmological objects such as our Galaxy. Semi-analytical models, built on top of such merger trees, are a co…
