المؤلفون: Forrest, Ben, Lemaux, Brian C., Shah, Ekta A., Staab, Priti, Gal, Roy R., Lubin, Lori M., Cooper, M. C., Cucciati, Olga, Hung, Denise, McConachie, Ian, Muzzin, Adam, Wilson, Gillian, Bardelli, Sandro, Cassarà, Letizia P., Chang, Wenjun, Giddings, Finn, Golden-Marx, Emmet, Hathi, Nimish, Stawinski, Stephanie M. Urbano, Zucca, Elena

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: We present an analysis of the number density of galaxies as a function of stellar mass (i.e., the stellar mass function, SMF) in the COSMOS field at z~3.3, making a comparison between the SMF in overdense environments and the SMF in the coeval field. In particular, this region contains the Elent\'ari proto-supercluster, a system of 6 extended overdensities spanning ~70 cMpc on a side. A clear difference is seen in the high-mass slope of these SMFs, with overdense regions showing an increase in the ratio of high-mass galaxies to low-mass galaxies relative to the field, indicating a more rapid build-up of stellar mass in overdense environments. This result qualitatively agrees with analyses of clusters at z~1, though the differences between protocluster and field SMFs at z~3.3 are smaller. While this is consistent with overdensities enhancing the evolution of their member galaxies, potentially through increased merger rates, whether this enhancement begins in protocluster environments or even earlier in group environments is still unclear. Though the measured fractions of quiescent galaxies between the field and overdense environments do not vary significantly, implying that this stellar mass enhancement is ongoing and any starbursts triggered by merger activity have not yet quenched, we note that spectroscopic observations are biased towards star-forming populations, particularly for low-mass galaxies. If mergers are indeed responsible, high resolution imaging of Elent\'ari and similar structures at these early epochs should then reveal increased merger rates relative to the field. Larger samples of well-characterized overdensities are necessary to draw broader conclusions in these areas.
Comment: 15 pages, 8 figures, plus references and appendices. Submitted to ApJ, posted after responding to referee comments. Further comments welcome

الوصول الحر: http://arxiv.org/abs/2405.18491Test

المؤلفون: Forrest, Ben, Lemaux, Brian C., Shah, Ekta, Staab, Priti, McConachie, Ian, Cucciati, Olga, Gal, Roy R., Hung, Denise, Lubin, Lori M., Cassarà, Letizia P., Cassata, Paolo, Chang, Wenjun, Cooper, M. C., Decarli, Roberto, Gomez, Percy, Gururajan, Gayathri, Hathi, Nimish, Kashino, Daichi, Marchesini, Danilo, Marsan, Z. Cemile, McDonald, Michael, Muzzin, Adam, Shen, Lu, Stawinski, Stephanie Urbano, Talia, Margherita, Vergani, Daniela, Wilson, Gillian, Zamorani, Giovanni

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: Motivated by spectroscopic confirmation of three overdense regions in the COSMOS field at $z\sim3.35$, we analyze the uniquely deep multi-wavelength photometry and extensive spectroscopy available in the field to identify any further related structure. We construct a three dimensional density map using the Voronoi tesselation Monte Carlo method and find additional regions of significant overdensity. Here we present and examine a set of six overdense structures at $3.20M$_\odot$, and is modeled to virialize at $z\sim1.5-2.0$. These structures contain ten overdense peaks with $>5\sigma$ overdensity separated by up to 70 cMpc, suggestive of a proto-supercluster similar to the Hyperion system at $z\sim2.45$. Upcoming photometric surveys with JWST such as COSMOS-Web, and further spectroscopic follow-up will enable more extensive analysis of the evolutionary effects that such an environment may have on its component galaxies at these early times.
Comment: Accepted for publication in MNRAS. 7 pages, 3 figures, 3 tables

الوصول الحر: http://arxiv.org/abs/2307.15113Test

المؤلفون: Fuskeland, U., Kaplan, A., Wehus, I. K., Eriksen, H. K., Christensen, P. R., von Hausegger, S., Liu, H., Lubin, P. M., Meinhold, P. R., Naselsky, P., Thommesen, H., Zonca, A.

المصدر: A&A, 684, A128 (2024)

مصطلحات موضوعية: Astrophysics - Cosmology and Nongalactic Astrophysics

الوصف: We present tensor-to-scalar ratio forecasts for GreenPol, a hypothetical ground-based B-mode experiment aiming to survey the cleanest regions of the Northern Galactic Hemisphere at five frequencies between 10 and 44 GHz. Its primary science goal would be to measure large-scale CMB polarization fluctuations at multipoles $\ell \lesssim 500$, and thereby constrain the primordial tensor-to-scalar ratio. The observations for the suggested experiment would take place at the Summit Station (72deg N, 38deg W) on Greenland, at an altitude of 3216 m above sea level. In this paper we simulate various experimental setups, and derive limits on the tensor-to-scalar ratio after CMB component separation using a Bayesian component separation implementation called Commander. When combining the proposed experiment with Planck HFI observations for constraining polarized thermal dust emission, we find a projected limit of r<0.02 at 95 % confidence for the baseline configuration. This limit is very robust with respect to a range of important experimental parameters, including sky coverage, detector weighting, foreground priors etc. Overall, GreenPol would have the possibility to provide deep CMB polarization measurements of the Northern Galactic Hemisphere at low frequencies.
Comment: 10 pages, 8 figures. Published in A&A

الوصول الحر: http://arxiv.org/abs/2306.13043Test

المؤلفون: Shen, Lu, Lemaux, Brian C., Lubin, Lori M., Liu, Guilin, Béthermin, Matthieu, Boquien, Médéric, Cucciati, Olga, Fèvre, Olivier Le, Talia, Margherita, Vergani, Daniela, Zamorani, Gianni, Faisst, Andreas L., Ginolfi, Michele, Gruppioni, Carlotta, Jones, Gareth C., Bardelli, Sandro, Hathi, Nimish, Koekemoer, Anton M., Romano, Michael, Schaerer, Daniel, Zucca, Elena, Fang, Wenjuan, Forrest, Ben, Gal, Roy, Hung, Denise, Shah, Ekta A., Staab, Priti, Vanderhoof, Brittany, Ibar, Eduardo

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: We present the radio properties of 66 spectroscopically-confirmed normal star-forming galaxies (SFGs) at $4.4Comment: Accepted for publication in Astrophysical Journal, 22 pages, 5 figure

الوصول الحر: http://arxiv.org/abs/2207.07137Test

المؤلفون: Vanderhoof, Brittany N., Faisst, A. L., Shen, L., Lemaux, B. C., Béthermin, M., Capak, P. L., Cassata, P., Fèvre, O. Le, Schaerer, D., Silverman, J., Yan, L., Boquien, M., Gal, R., Kartaltepe, J., Lubin, L. M., Dessauges-Zavadsky, M., Fudamoto, Y., Ginolfi, M., Hathi, N. P., Jones, G. C., Koekemoer, A. M., Narayanan, D., Romano, M., Talia, M., Vergani, D., Zamorani, G.

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: We present $10$ main-sequence ALPINE galaxies (log($M/M_{\odot}$) = 9.2-11.1 and ${\rm SFR}=23-190\,{\rm M_{\odot}\,yr^{-1}}$) at $z\sim4.5$ with optical [OII] measurements from Keck/MOSFIRE spectroscopy and Subaru/MOIRCS narrow-band imaging. This is the largest such multi-wavelength sample at these redshifts, combining various measurements in the ultra-violet, optical, and far-infrared including [CII]$_{158{\rm \mu m}}$ line emission and dust continuum from ALMA and H$\alpha$ emission from Spitzer photometry. For the first time, this unique sample allows us to analyze the relation between [OII] and total star-formation rate (SFR) and the interstellar medium (ISM) properties via [OII]/[CII] and [OII]/\halpha luminosity ratios at $z\sim4.5$. The [OII]$-$SFR relation at $z\sim4.5$ cannot be described using standard local descriptions, but is consistent with a metal-dependent relation assuming metallicities around $50\%$ solar. To explain the measured dust-corrected luminosity ratios of $L[OII]/L[CII] \sim 0.98^{+0.21}_{-0.22}$ and $L[OII]/LHa \sim -0.22^{+0.13}_{-0.15}$ for our sample, ionization parameters $\log(U)< -2$ and electron densities $\log(\rm n_e / {\rm [cm^{-3}]}) \sim 2.5-3$ are required. The former is consistent with galaxies at $z\sim2-3$, however lower than at $z>6$. The latter may be slightly higher than expected given the galaxies' specific SFR. The analysis of this pilot sample suggests that typical log($ M/M_{\odot})$ > 9 galaxies at $z\sim4.5$ to have broadly similar ISM properties as their descendants at $z\sim2$ and suggest a strong evolution of ISM properties since the Epoch of Reionization at $z>6$.
Comment: 14 pages, 8 figures, Accepted for publication to MNRAS

الوصول الحر: http://arxiv.org/abs/2201.03587Test

المؤلفون: Shen, Lu, Lemaux, Brian C., Lubin, Lori M., Cucciati, Olga, Fevre, Olivier Le, Liu, Guilin, Fang, Wenjuan, Pelliccia, Debora, Tomczak, Adam, McKean, John, Miller, Neal A., Fassnacht, Christopher D., Gal, Roy, Hung, Denise, Hathi, Nimish, Bardelli, Sandro, Vergani, Daniela, Zucca, Elena

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: Radio Active Galactic Nuclei (RAGNs) are mainly found in dense structures (i.e., clusters/groups) at redshifts of z$<$2 and are commonly used to detect protoclusters at higher redshift. Here, we attempt to study the host and environmental properties of two relatively faint ($\mathrm L_\mathrm{1.4GHz} \sim10^{25}$ W Hz$^{-1}$) RAGNs in a known protocluster at z=3.3 in the PCl J0227-0421 field, detected using the latest radio observation obtained as part of the Observations of Redshift Evolution in Large-Scale Environments (ORELSE) Survey. Using new spectroscopic observations obtained from Keck/MOSFIRE as part of the Charting Cluster Construction with the VIMOS Ultra-Deep Survey (VUDS) and ORELSE (C3VO) survey and previous spectroscopic data obtained as part of the VIMOS-VLT Deep Survey (VVDS) and VUDS, we revise the three-dimensional overdensity field around this protocluster. The protocluster is embedded in a large scale overdensity protostructure. This protostructure has an estimated total mass of $\sim$2.6$\times10^{15} M_\odot$ and contains several overdensity peaks. Both RAGNs are hosted by very bright and massive galaxies, while their hosts show extreme differences color, indicating that they have different ages and are in different evolutionary stages. Furthermore, we find that they are not in the most locally dense parts of the protostructure, but are fairly close to the centers of their parent overdensity peaks. We propose a scenario where merging might already have happened in both cases, which lowered the local density of their surrounding area and boosted their stellar mass. This work is the first time that two RAGNs at low luminosity have been found and studied within a high redshift protostructure.
Comment: 23 pages, 11 figures, 4 tables, accepted by ApJ

الوصول الحر: http://arxiv.org/abs/2103.03441Test

المؤلفون: Hung, D., Lemaux, B. C., Gal, R. R., Tomczak, A. R., Lubin, L. M., Cucciati, O., Pelliccia, D., Shen, L., Fèvre, O. Le, Zamorani, G., Wu, P-F., Kocevski, D. D., Fassnacht, C. D., Squires, G. K.

مصطلحات موضوعية: Astrophysics - Cosmology and Nongalactic Astrophysics

الوصف: We present a new mass function of galaxy clusters and groups using optical/near-infrared wavelength spectroscopic and photometric data from the Observations of Redshift Evolution in Large-Scale Environments (ORELSE) survey. At $z\sim1$, cluster mass function studies are rare regardless of wavelength and have never been attempted from an optical/near-infrared perspective. This work serves as a proof of concept that $z\sim1$ cluster mass functions are achievable without supplemental X-ray or Sunyaev-Zel'dovich (SZ) data. Measurements of the cluster mass function provide important contraints on cosmological parameters and are complementary to other probes. With ORELSE, a new cluster finding technique based on Voronoi tessellation Monte-Carlo (VMC) mapping, and rigorous purity and completeness testing, we have obtained $\sim$240 galaxy overdensity candidates in the redshift range $0.55M/M_{\odot})<14.8$. This mass range is comparable to existing optical cluster mass function studies for the local universe. Our candidate numbers vary based on the choice of multiple input parameters related to detection and characterization in our cluster finding algorithm, which we incorporated into the mass function analysis through a Monte-Carlo scheme. We find cosmological constraints on the matter density of $\Omega_{m} = 0.250^{+0.104}_{-0.099}$ and on the amplitude of fluctuations of $\sigma_{8} = 1.150^{+0.260}_{-0.163}$. While our $\Omega_{m}$ value is close to concordance, our $\sigma_{8}$ value is $\sim2\sigma$ higher because of the inflated observed number densities compared to theoretical mass function models owing to how our survey targeted overdense regions. With Euclid and several other large, unbiased optical surveys on the horizon, VMC mapping will enable optical/NIR cluster cosmology at redshifts much higher than what has been possible before.
Comment: 13 pages, 8 figures, submitted to MNRAS

الوصول الحر: http://arxiv.org/abs/2101.02215Test

المؤلفون: Shen, Lu, Liu, Guilin, Zhang, Mengfei, Lemaux, Brian C., Lubin, Lori M., Pelliccia, Debora, Moravec, Emily, Golden-Marx, Emmet G., Zhou, Hongyan, Fang, Wenjuan, Tomczak, Adam, McKean, John, Miller, Neal A., Fassnacht, Christopher D., Wu, Po-Feng, Kocevski, Dale D., Gal, Roy R., Hung, Denise, Squires, Gordon K

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: Recent hydrodynamic simulations and observations of radio jets have shown that the surrounding environment has a large effect on their resulting morphology. To investigate this we use a sample of 50 Extended Radio Active Galactic Nuclei (ERAGN) detected in the Observations of Redshift Evolution in Large Scale Environments (ORELSE) survey. These sources are all successfully cross-identified to galaxies within a redshift range of $0.55 \leq z \leq 1.35$, either through spectroscopic redshifts or accurate photometric redshifts. We find that ERAGN are more compact in high-density environments than those in low-density environments at a significance level of 4.5$\sigma$. Among a series of internal properties under our scrutiny, only the radio power demonstrates a positive correlation with their spatial extent. After removing the possible radio power effect, the difference of size in low- and high-density environments persists. In the global environment analyses, the majority (86\%) of high-density ERAGN reside in the cluster/group environment. In addition, ERAGN in the cluster/group central regions are preferentially compact with a small scatter in size, compared to those in the cluster/group intermediate regions and fields. In conclusion, our data appear to support the interpretation that the dense intracluster gas in the central regions of galaxy clusters plays a major role in confining the spatial extent of radio jets.

الوصول الحر: http://arxiv.org/abs/2009.03343Test

المؤلفون: Lemaux, B. C., Cucciati, O., Fèvre, O. Le, Zamorani, G., Lubin, L. M., Hathi, N., Ilbert, O., Pelliccia, D., Amorín, R., Bardelli, S., Cassata, P., Gal, R. R., Garilli, B., Guaita, L., Giavalisco, M., Hung, D., Koekemoer, A., Maccagni, D., Pentericci, L., Ribeiro, B., Schaerer, D., Shah, E., Shen, L., Staab, P., Talia, M., Thomas, R., Tomczak, A. R., Tresse, L., Vanzella, E., Vergani, D., Zucca, E.

المصدر: A&A 662, A33 (2022)

مصطلحات موضوعية: Astrophysics - Astrophysics of Galaxies

الوصف: Utilizing spectroscopic observations taken for the VIMOS Ultra-Deep Survey (VUDS), new observations from Keck/DEIMOS, and publicly available observations of large samples of star-forming galaxies, we report here on the relationship between the star formation rate (SFR) and the local environment ($\delta_{gal}$) of galaxies in the early universe ($2Comment: v2, 24 pages, nine figures, accepted to A&A after minor changes to language and formatting

الوصول الحر: http://arxiv.org/abs/2009.03324Test

المؤلفون: Planck Collaboration, Akrami, Y., Andersen, K. J., Ashdown, M., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Benabed, K., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bond, J. R., Borrill, J., Burigana, C., Butler, R. C., Calabrese, E., Casaponsa, B., Chiang, H. C., Colombo, L. P. L., Combet, C., Crill, B. P., Cuttaia, F., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Di Valentino, E., Diego, J. M., Doré, O., Douspis, M., Dupac, X., Eriksen, H. K., Fernandez-Cobos, R., Finelli, F., Frailis, M., Fraisse, A. A., Franceschi, E., Frolov, A., Galeotta, S., Galli, S., Ganga, K., Gerbino, M., Ghosh, T., González-Nuevo, J., Górski, K. M., Gruppuso, A., Gudmundsson, J. E., Handley, W., Helou, G., Herranz, D., Hildebrandt, S. R., Hivon, E., Huang, Z., Jaffe, A. H., Jones, W. C., Keihänen, E., Keskitalo, R., Kiiveri, K., Kim, J., Kisner, T. S., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lasenby, A., Lattanzi, M., Lawrence, C. R., Jeune, M. Le, Levrier, F., Liguori, M., Lilje, P. B., Lilley, M., Lindholm, V., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maino, D., Mandolesi, N., Marcos-Caballero, A., Maris, M., Martin, P. G., Martínez-González, E., Matarrese, S., Mauri, N., McEwen, J. D., Meinhold, P. R., Mennella, A., Migliaccio, M., Mitra, S., Molinari, D., Montier, L., Morgante, G., Moss, A., Natoli, P., Paoletti, D., Partridge, B., Patanchon, G., Pearson, D., Pearson, T. J., Perrotta, F., Piacentini, F., Polenta, G., Rachen, J. P., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Ruiz-Granados, B., Salvati, L., Savelainen, M., Scott, D., Sirignano, C., Sirri, G., Spencer, L. D., Suur-Uski, A. -S., Svalheim, T. L., Tauber, J. A., Tavagnacco, D., Tenti, M., Terenzi, L., Thommesen, H., Toffolatti, L., Tomasi, M., Tristram, M., Trombetti, T., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wehus, I. K., Zacchei, A., Zonca, A.

المصدر: A&A 643, A42 (2020)

مصطلحات موضوعية: Astrophysics - Cosmology and Nongalactic Astrophysics

الوصف: We present the NPIPE processing pipeline, which produces calibrated frequency maps in temperature and polarization from data from the Planck Low Frequency Instrument (LFI) and High Frequency Instrument (HFI) using high-performance computers. NPIPE represents a natural evolution of previous Planck analysis efforts, and combines some of the most powerful features of the separate LFI and HFI analysis pipelines. The net effect of the improvements is lower levels of noise and systematics in both frequency and component maps at essentially all angular scales, as well as notably improved internal consistency between the various frequency channels. Based on the NPIPE maps, we present the first estimate of the Solar dipole determined through component separation across all nine Planck frequencies. The amplitude is ($3366.6 \pm 2.7$)$\mu$K, consistent with, albeit slightly higher than, earlier estimates. From the large-scale polarization data, we derive an updated estimate of the optical depth of reionization of $\tau = 0.051 \pm 0.006$, which appears robust with respect to data and sky cuts. There are 600 complete signal, noise and systematics simulations of the full-frequency and detector-set maps. As a Planck first, these simulations include full time-domain processing of the beam-convolved CMB anisotropies. The release of NPIPE maps and simulations is accompanied with a complete suite of raw and processed time-ordered data and the software, scripts, auxiliary data, and parameter files needed to improve further on the analysis and to run matching simulations.
Comment: 97 pages, 93 figures and 16 tables, abstract abridged for arXiv submission, accepted for publication in A&A

الوصول الحر: http://arxiv.org/abs/2007.04997Test