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7 results on '"Cosmology:large-scale structure of universe"'

1. Protoclusters as drivers of stellar mass growth in the early Universe, a case study: Taralay – a massive protocluster at z ∼ 4.57.

Author

Staab, Priti, Lemaux, Brian C, Forrest, Ben, Shah, Ekta, Cucciati, Olga, Lubin, Lori, Gal, Roy R, Hung, Denise, Shen, Lu, Giddings, Finn, Khusanova, Yana, Zamorani, Giovanni, Bardelli, Sandro, Cassara, Letizia Pasqua, Cassata, Paolo, Chiang, Yi-Kuan, Fudamoto, Yoshinobu, Fukushima, Shuma, Garilli, Bianca, and Giavalisco, Mauro

Subjects
*STAR formation, *STELLAR mass, *GALACTIC evolution, *GALAXIES, *GALAXY clusters, *GALACTIC redshift, UNIVERSE
Abstract

Simulations predict that the galaxy populations inhabiting protoclusters may contribute considerably to the total amount of stellar mass growth of galaxies in the early universe. In this study, we test these predictions observationally, using the Taralay protocluster (formerly PCl J1001+0220) at z ∼ 4.57 in the COSMOS field. With the Charting Cluster Construction with VUDS and ORELSE (C3VO) survey, we spectroscopically confirmed 44 galaxies within the adopted redshift range of the protocluster (4.48 < z < 4.64) and incorporate an additional 18 galaxies from ancillary spectroscopic surveys. Using a density mapping technique, we estimate the total mass of Taralay to be ∼1.7 × 1015 M⊙, sufficient to form a massive cluster by the present day. By comparing the star formation rate density (SFRD) within the protocluster (SFRDpc) to that of the coeval field (SFRDfield), we find that SFRDpc surpasses the SFRDfield by Δlog (SFRD/M⊙yr−1 Mpc−3) = 1.08 ± 0.32 (or ∼12 ×). The observed contribution fraction of protoclusters to the cosmic SFRD adopting Taralay as a proxy for typical protoclusters is |$33.5~{{\ \rm per\ cent}}^{+8.0~{{\ \rm per\ cent}}}_{-4.3~{{\ \rm per\ cent}}}$|⁠ , a value ∼2σ higher than the predictions from simulations. Taralay contains three peaks that are 5σ above the average density at these redshifts. Their SFRD is ∼0.5 dex higher than the value derived for the overall protocluster. We show that 68 per cent of all star formation in the protocluster takes place within these peaks, and that the innermost regions of the peaks encase |$\sim 50~{{\ \rm per\ cent}}$| of the total star formation in the protocluster. This study strongly suggests that protoclusters drive stellar mass growth in the early universe and that this growth may proceed in an inside-out manner. [ABSTRACT FROM AUTHOR]

Published
2024
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2. cosmic environment overtakes the local density in shaping galaxy star formation.

Author

Ren, Jian, Pan, Zhizheng, Zheng, X Z, Qin, Jianbo, Shi, D D, Gonzalez, Valentino, Bian, Fuyan, Huang, Jia-Sheng, Fang, Min, Liu, Wenhao, Wen, Run, Zhang, Yuheng, Qiao, Man, and Liu, Shuang

Subjects
*STAR formation, *GALACTIC evolution, *GALAXY formation, *GALAXY clusters, *STELLAR mass, *STELLAR density (Stellar population), *GALAXIES
Abstract

The gas supply from the cosmic web is the key to sustain star formation in galaxies. It remains to be explored how the cosmic large-scale structure (LSS) effects on galaxy evolution at given local environments. We examine galaxy-specific star formation rate as a function of local density in a LSS at z  = 0.735 in the Extended Chandra Deep Field South. The LSS is mapped by 732 galaxies with R < 24 mag and redshift at 0.72 ≤ z ≤ 0.75 collected from the literature and our spectroscopic observations with Magellan/IMACS, consisting of five galaxy clusters/groups and surrounding filaments over an area of 23.9 × 22.7 co-moving Mpc2. The spread of spectroscopic redshifts corresponds a velocity dispersion of 494 km s−1, indicating the LSS likely to be a thin sheet with a galaxy density ≳ 3.9 times that of the general field. These clusters/groups in this LSS mostly exhibit elongated morphologies and multiple components connected with surrounding filaments. Strikingly, we find that star-forming galaxies in the LSS keep star formation at the same level as field, and show no dependence on local density but stellar mass. Meanwhile, an increasing fraction of quiescent galaxies is detected at increasing local density in both the LSS and the field, consistent with the expectation that galaxy mass and local dense environment hold the key to quench star formation. Combined together, we conclude that the cosmic environment of the LSS overtakes the local environment in remaining galaxy star formation to the level of the field. [ABSTRACT FROM AUTHOR]

Published
2022
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3. Multipole expansion for 21cm Intensity Mapping power spectrum: forecasted cosmological parameters estimation for the SKA Observatory

Author

Maria Berti, Marta Spinelli, and Matteo Viel

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, cosmology: cosmological parameters, cosmology: large-scale structure of Universe, radio lines: general, cosmological parameters, cosmology:large-scale structure of Universe, radio lines:general [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The measurement of the large scale distribution of neutral hydrogen in the late Universe, obtained with radio telescopes through the hydrogen 21cm line emission, has the potential to become a key cosmological probe in the upcoming years. We explore the constraining power of 21cm intensity mapping observations on the full set of cosmological parameters that describe the $\Lambda$CDM model. We assume a single-dish survey for the SKA Observatory and simulate the 21cm linear power spectrum monopole and quadrupole within six redshift bins in the range $z=0.25-3$. Forecasted constraints are computed numerically through Markov Chain Monte Carlo techniques. We extend the sampler \texttt{CosmoMC} by implementing the likelihood function for the 21cm power spectrum multipoles. We assess the constraining power of the mock data set alone and combined with Planck 2018 CMB observations. We include a discussion on the impact of extending measurements to non-linear scales in our analysis. We find that 21cm multipoles observations alone are enough to obtain constraints on the cosmological parameters comparable with other probes. Combining the 21cm data set with CMB observations results in significantly reduced errors on all the cosmological parameters. The strongest effect is on $\Omega_ch^2$ and $H_0$, for which the error is reduced by almost a factor four. The percentage errors we estimate are $\sigma_{\Omega_ch^2} = 0.25\%$ and $\sigma_{H_0} = 0.16\%$, to be compared with the Planck only results $\sigma_{\Omega_ch^2} = 0.99\%$ and $\sigma_{H_0} = 0.79\%$. We conclude that 21cm SKAO observations will provide a competitive cosmological probe, complementary to CMB and, thus, pivotal for gaining statistical significance on the cosmological parameters constraints, allowing a stress test for the current cosmological model., Comment: 16 pages, 9 figures

Published
2022

4. Characterising large-scale structure with the REFLEX II cluster survey.

Author

Chon, Gayoung, van de Weygaert, R., Shandarin, S., Saar, E., and Einasto, J.

Abstract

We study the large-scale structure with superclusters from the REFLEX X-ray cluster survey together with cosmological N-body simulations. It is important to construct superclusters with criteria such that they are homogeneous in their properties. We lay out our theoretical concept considering future evolution of superclusters in their definition, and show that the X-ray luminosity and halo mass functions of clusters in superclusters are found to be top-heavy, different from those of clusters in the field. We also show a promising aspect of using superclusters to study the local cluster bias and mass scaling relation with simulations. [ABSTRACT FROM PUBLISHER]

Published
2014
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5. A deep study of the most massive galaxy cluster at z>1.5.

Subjects
GALAXY clusters, REDSHIFT, STAR formation, STELLAR evolution
Abstract

The X-ray satellite Chandra is the only telescope able to provide high-resolution (~1 arcsec) images in the X-ray band (0.5-10 keV). An international collaboration met in Janu-ary 2014 at the Villa Il Gioiello to discuss the Chandra Large Program on the high redshift (z=1.58) galaxy cluster XDCP J0044.0-2033, constituting the deepest X-ray observation cur-rently achieved on a massive, high redshift cluster. Thanks to this unprecedented observa-tion, coupled to a wealth of optical and IR data, we are able to investigate the properties of the Intra Cluster Medium, star formation and nuclear activity in the cluster galaxies, and to measure the total mass of the cluster, for the first time at such a high redshift. [ABSTRACT FROM AUTHOR]

Published
2014
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6. The zCOSMOS Redshift Survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z~1

Author

Tasca L. A. M., Kneib J. P., Iovino A., Le Fèvre O., Kova, #269, Bolzonella M., Lilly S. J., Abraham R. G., Cassata P., Guzzo L., Tresse L., Zamorani G., Capak P., Garilli B., Scodeggio M., Sheth K., Zucca E., Carollo C. M., Contini T., Mainieri V., Renzini A., Bardelli S., Bongiorno A., Caputi K., Coppa G., de La Torre S., de Ravel L., Franzetti P., Kampczyk P., Knobel C., Koekemoer A. M., Lamareille F., Le Borgne J. F., Le Brun V., Maier C., Mignoli M., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Vergani D., Tanaka M., Abbas U., Bottini D., Cappi A., Ilbert O., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., Scaramella R., Scarlata C., CUCCIATI, OLGA, CIMATTI, ANDREA, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), AUTRES, INAF - Osservatorio Astronomico di Bologna (OABO), Mathématiques - Analyse, Probabilités, Modélisation - Orléans (MAPMO), Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), INAF- Milano, California Institute of Technology (CALTECH), Spitzer Science Center, California Institute of Technology, Pasadena, University of Chicago, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Space Telescope Science Institute (STSci), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Human Genetics Center, The University of Texas Health Science Center at Houston (UTHealth), School of Biotechnology and Biomolecular Sciences, University of New South Wales [Sydney] (UNSW), Centre de Physique Théorique - UMR 6207 (CPT), Université de la Méditerranée - Aix-Marseille 2-Université de Provence - Aix-Marseille 1-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Université de Provence - Aix-Marseille 1-Université de la Méditerranée - Aix-Marseille 2, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Tasca L. A. M., Kneib J.-P., Iovino A., Le Fèvre O., Kova&#269, K., Bolzonella M., Lilly S. J., Abraham R. G., Cassata P., Cucciati O., Guzzo L., Tresse L., Zamorani G., Capak P., Garilli B., Scodeggio M., Sheth K., Zucca E., Carollo C. M., Contini T., Mainieri V., Renzini A., Bardelli S., Bongiorno A., Caputi K., Coppa G., de La Torre S., de Ravel L., Franzetti P., Kampczyk P., Knobel C., Koekemoer A. M., Lamareille F., Le Borgne J.-F., Le Brun V., Maier C., Mignoli M., Pello R., Peng Y., Perez Montero E., Ricciardelli E., Silverman J. D., Vergani D., Tanaka M., Abbas U., Bottini D., Cappi A., Cimatti A., Ilbert O., Leauthaud A., Maccagni D., Marinoni C., McCracken H. J., Memeo P., Meneux B., Oesch P., Porciani C., Pozzetti L., Scaramella R., and Scarlata C.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Galaxy:formation, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Galaxies:structure, Galaxy group, 0103 physical sciences, Cosmology:large-scale structure of universe, Galaxies:distances and redshifts, Galaxies:evolution, Galaxies:fundamental parameters, Astronomy and Astrophysics, Space and Planetary Science, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Redshift survey, Galaxy, Universe, Redshift, 13. Climate action, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

For more than two decades we have known that galaxy morphological segregation is present in the Local Universe. It is important to see how this relation evolves with cosmic time. To investigate how galaxy assembly took place with cosmic time, we explore the evolution of the morphology-density relation up to redshift z~1 using about 10000 galaxies drawn from the zCOSMOS Galaxy Redshift Survey. Taking advantage of accurate HST/ACS morphologies from the COSMOS survey, of the well-characterised zCOSMOS 3D environment, and of a large sample of galaxies with spectroscopic redshift, we want to study here the evolution of the morphology-density relation up to z~1 and its dependence on galaxy luminosity and stellar mass. The multi-wavelength coverage of the field also allows a first study of the galaxy morphological segregation dependence on colour. We further attempt to disentangle between processes that occurred early in the history of the Universe or late in the life of galaxies. The zCOSMOS field benefits of high-resolution imaging in the F814W filter from the Advanced Camera for Survey (ACS). We use standard morphology classifiers, optimised for being robust against band-shifting and surface brightness dimming, and a new, objective, and automated method to convert morphological parameters into early, spiral, and irregular types. We use about 10000 galaxies down to I_AB=22.5 with a spectroscopic sampling rate of 33% to characterise the environment of galaxies up to z~1 from the 100 kpc scales of galaxy groups up to the 100 Mpc scales of the cosmic web. ABRIDGED, Comment: 23 pages, 12 figures, accepted for publication in Astronomy and Astrophysics

Published
2009
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7. Search for X-ray signatures of the cosmic web in superclusters.

Author

Madej, Oliwia and Werner, Norbert

Subjects
*GALAXY clusters, *X-ray spectroscopy, *SPECTRUM analysis, *ASTRONOMICAL observations, *SUPERCLUSTERS
Abstract

We investigated an X-ray selected sample of galaxy clusters in terms of their interactions with the large-scale structure filaments. The analysis was based on the X-ray observations performed by the XMM-Newton satellite over the last 10 years. Nine clusters in the sample of forty show excess emission in the direction of the cosmic web filaments. Since the excess emission is present within the cluster virial radius, we suggest that it is an evidence of the gas moving towards the cluster along the primordial filament. [ABSTRACT FROM AUTHOR]

Published
2010
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