Antonio D. Montero-Dorta

Federico Santa María Technical University

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Ginevra Favole

Instituto de Astrofísica de Canarias

A. Bolton

Community Science and Data Center

M. Celeste Artale

Istituto Nazionale di Fisica Nucleare, Sezione di Padova

L. Raul Abramo

Universidade de São Paulo

Francisco Prada

Consejo Superior de Investigaciones Científicas

David J. Schlegel

Lawrence Berkeley National Laboratory

Ariel G. Sánchez

Max Planck Institute for Extraterrestrial Physics

Sergio Rodríguez-Torres

Universidad Autónoma de Madrid

Joel R. Brownstein

University of Utah

Cameron K. McBride

Vanderbilt University

Cooperative Institutions

Centre National de la Recherche Scientifique

Universidade de São Paulo

Max Planck Society

Consejo Superior de Investigaciones Científicas

Max Planck Institute for Astronomy

Instituto de Astrofísica de Canarias

Museu de Astronomia e Ciências Afins

Instituto de Astrofísica de Andalucía

University of California, Berkeley

Lawrence Berkeley National Laboratory

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The physical origins of low-mass spin bias

Monthly Notices of the Royal Astronomical Society (2020)

Beatriz Tucci Antonio D. Montero-Dorta L. Raul Abramo Gabriela Sato-Polito M. Celeste Artale

At $z=0$, higher-spin haloes with masses above $\log(\text{M}_{\text{c}}/h^{-1}\text{M}_\odot)\simeq 11.5$ have a higher bias than lower-spin haloes of the same mass. However, this trend is known to invert below this characteristic crossover mass, $\text{M}_{\text{c}}$. In this paper, we measure the redshift evolution and scale dependence of halo spin bias at the low-mass end and demonstrate that the inversion of the signal is entirely produced by the effect of splashback haloes. These low-mass haloes tend to live in the vicinity of significantly more massive haloes, thus sharing their large-scale bias properties. We further show that the location of the redshift-dependent crossover mass scale $\text{M}_{\text{c}}(z)$ is completely determined by the relative abundance of splashbacks in the low- and high-spin subpopulations. Once splashback haloes are removed from the sample, the intrinsic mass dependence of spin bias is recovered. Since splashbacks have been shown to account for some of the assembly bias signal at the low-mass end, our results unveil a specific link between two different secondary bias trends: spin bias and assembly bias.

Low Mass

Halo effect

10.1093/mnras/staa3319

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Citations (17)

Tracking the evolution of satellite galaxies: mass stripping and dark-matter deficient galaxies

Monthly Notices of the Royal Astronomical Society (2023)

Antonio D. Montero-Dorta Facundo Rodríguez M. Celeste Artale R. J. E. Smith Jonás Chaves-Montero

ABSTRACT Satellite galaxies undergo a variety of physical processes when they are accreted by groups and clusters, often resulting in the loss of baryonic and dark matter (DM) mass. In this work, we evaluate the predictions from the IllustrisTNG hydrodynamical simulation regarding the evolution of the matter content of satellites, focusing on a population that are accreted at z > 1 and retain their identity as satellites down to z = 0. At fixed host halo mass, the amount of DM and stellar mass stripped depends mostly on the pericentric distance, dperi, here normalized by host halo virial radius. The closest encounters result in significant loss of DM, with subhaloes retaining between 20 and a few per cent of their z = 1 mass. At fixed dperi, DM mass stripping seems more severe in lower mass haloes. Conversely, the average satellite in higher mass haloes has its stellar mass growth halted earlier, having lost a higher fraction of stellar mass by z = 0. We also show that mass stripping has a strong impact on the quenched fractions. The IllustrisTNG boxes are qualitatively consistent in these predictions, with quantitative differences mostly originating from the distinct subhalo mass ranges covered by the boxes. Finally, we have identified DM-deficient systems in all TNG boxes. These objects are preferentially found in massive clusters (Mhost ≳ 1013 M⊙), had very close encounters with their central galaxies ($d_{\rm peri}\simeq 0.05\, R_{\rm vir}$), and were accreted at high redshift (zinfall ≳ 1.4), reinforcing the notion that tidal stripping is responsible for their remarkable lack of DM.

Satellite galaxy

Stellar mass

Virial mass

Mass fraction

10.1093/mnras/stad3268

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The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the large-scale two-point correlation function

Monthly Notices of the Royal Astronomical Society (2012)

Ariel G. Sánchez Claudia G. Scóccola Ashley J. Ross Will J. Percival Marc Manera

We obtain constraints on cosmological parameters from the spherically averaged redshiftspace correlation function of the CMASS Data Release 9 (DR9) sample of the Baryonic Oscillation Spectroscopic Survey (BOSS).We combine this information with additional data from recent cosmic microwave background (CMB), supernova and baryon acoustic oscillation measurements.Our results show no significant evidence of deviations from the standard flat cold dark matter model, whose basic parameters can be specified by m = 0.285 ± 0.009, 100 b = 4.59 ± 0.09, n s = 0.961 ± 0.009, H 0 = 69.4± 0.8 km s -1 Mpc -1 and σ 8 = 0.80 ± 0.02.The CMB+CMASS combination sets tight constraints on the curvature of the Universe, with k = -0.0043± 0.0049, and the tensor-to-scalar amplitude ratio, for which we find r < 0.16 at the 95 per cent confidence level (CL).These data show a clear signature of a deviation from scale invariance also in the presence of tensor modes, with n s < 1 at the 99.7 per cent CL.We derive constraints on the fraction of massive neutrinos of f ν < 0.049 (95 per cent CL), implying a limit of m ν < 0.51 eV.We find no signature of a deviation from a cosmological constant from the combination of all data sets, with a constraint of w DE = -1.033± 0.073 when this parameter is assumed time-independent, and no evidence of a departure from this value when it is allowed to evolve as w DE (a) = w 0 + w a (1a).The achieved accuracy on our cosmological constraints is a clear demonstration of the constraining power of current cosmological observations.

Cosmological constant

10.1111/j.1365-2966.2012.21502.x

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Citations (183)

Fibre assignment in next-generation wide-field spectrographs

Monthly Notices of the Royal Astronomical Society (2011)

Isaac Morales Antonio D. Montero-Dorta M. Azzaro F. Prada Justo Sánchez

We present an optimized algorithm for assigning fibres to targets in next-generation fibre-fed multi-object spectrographs. The method, which we have called the draining algorithm, ensures that the maximum number of targets in a given target field is observed in the first few tiles. Using randomly distributed targets and mock galaxy catalogues, we have estimated that the gain provided by the draining algorithm, compared to a random assignment, can be as much as 2 per cent for the first tiles. For a survey such as the Baryon Oscillation Spectroscopic Survey (BigBOSS), this would imply saving for observation several hundred thousand objects or, alternatively, reducing the covered area in ∼350 deg2. An important advantage of this method is that the fibre collision problem can be solved easily and in an optimal way. We also discuss the additional optimizations of the fibre-positioning process. In particular, we show that if we allow for the rotation of the focal plane, we can improve the efficiency of the process by ∼3.5–4.5 per cent, even if only small adjustments are permitted (up to 2°). For instruments that allow large rotations of the focal plane, the expected gain increases to ∼5–6 per cent. Therefore, these results strongly support the use of focal plane rotation in future spectrographs, as far as the efficiency of the fibre-positioning process is concerned. Finally, we discuss the implications of our optimizations and provide some basic hints for an optimal survey strategy, based on the number of targets per positioner.

Field of view

10.1111/j.1365-2966.2011.19774.x

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The BigBOSS Experiment

arXiv (Cornell University) (2011)

David J. Schlegel F. B. Abdalla Tara H. Abraham Christopher P. Ahn C. Allende Prieto

BigBOSS is a Stage IV ground-based dark energy experiment to study baryon acoustic oscillations (BAO) and the growth of structure with a wide-area galaxy and quasar redshift survey over 14,000 square degrees. It has been conditionally accepted by NOAO in response to a call for major new instrumentation and a high-impact science program for the 4-m Mayall telescope at Kitt Peak. The BigBOSS instrument is a robotically-actuated, fiber-fed spectrograph capable of taking 5000 simultaneous spectra over a wavelength range from 340 nm to 1060 nm, with a resolution R = 3000-4800. Using data from imaging surveys that are already underway, spectroscopic targets are selected that trace the underlying dark matter distribution. In particular, targets include luminous red galaxies (LRGs) up to z = 1.0, extending the BOSS LRG survey in both redshift and survey area. To probe the universe out to even higher redshift, BigBOSS will target bright [OII] emission line galaxies (ELGs) up to z = 1.7. In total, 20 million galaxy redshifts are obtained to measure the BAO feature, trace the matter power spectrum at smaller scales, and detect redshift space distortions. BigBOSS will provide additional constraints on early dark energy and on the curvature of the universe by measuring the Ly-alpha forest in the spectra of over 600,000 2.2 < z < 3.5 quasars. BigBOSS galaxy BAO measurements combined with an analysis of the broadband power, including the Ly-alpha forest in BigBOSS quasar spectra, achieves a FOM of 395 with Planck plus Stage III priors. This FOM is based on conservative assumptions for the analysis of broad band power (kmax = 0.15), and could grow to over 600 if current work allows us to push the analysis to higher wave numbers (kmax = 0.3). BigBOSS will also place constraints on theories of modified gravity and inflation, and will measure the sum of neutrino masses to 0.024 eV accuracy.

Baryon Acoustic Oscillations

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The manifestation of secondary bias on the galaxy population from IllustrisTNG300

Monthly Notices of the Royal Astronomical Society (2020)

Antonio D. Montero-Dorta M. Celeste Artale L. Raul Abramo Beatriz Tucci Nelson Padilla

We use the improved IllustrisTNG300 magneto-hydrodynamical cosmological simulation to revisit the effect that secondary halo bias has on the clustering of the central galaxy population. With a side length of 205 $h^{-1}$Mpc and significant improvements on the sub-grid model with respect to the previous Illustris boxes, IllustrisTNG300 allows us to explore the dependencies of galaxy clustering over a large cosmological volume and wide halo-mass range. We show, at high statistical significance, that the halo assembly bias signal (i.e., the secondary dependence of halo bias on halo formation redshift) manifests itself on the clustering of the central galaxy population when this is split by stellar mass, colour, specific star formation rate, and surface density. A significant detection is also obtained for galaxy size: at fixed halo mass, larger central galaxies are more tightly clustered than smaller central galaxies in haloes of mass M$_{\rm vir} \lesssim 10^{12.5}$ $h^{-1}$M$_{\odot}$. This effect, however, seems to be uncorrelated with halo formation time, unlike the rest of the secondary dependencies analysed. We also explore the transmission of the halo spin bias signal, i.e., the secondary dependence of halo bias on halo spin. Although galaxy spin retains little information about the total spin of the halo, the correlation is enough to produce a significant galaxy spin bias signal. We discuss possible ways to probe the spin bias effects with observations.

Satellite galaxy

10.1093/mnras/staa1624

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The DEEP2 Galaxy Redshift Survey: the red sequence AGN fraction and its environment and redshift dependence

Monthly Notices of the Royal Astronomical Society (2008)

Antonio D. Montero-Dorta Darren Croton Renbin Yan Michael C. Cooper Jeffery A. Newman

We measure the dependence of the active galactic nuclei (AGN) fraction on local environment at z∼ 1, using spectroscopic data taken from the DEEP2 Galaxy Redshift Survey, and Chandra X-ray data from the All-Wavelength Extended Groth Strip International Survey (AEGIS). To provide a clean sample of AGN, we restrict our analysis to the red sequence population; this also reduces additional colour–environment correlations. We find evidence that high-redshift LINERs in DEEP2 tend to favour higher density environments relative to the red population from which they are drawn. In contrast, Seyferts and X-ray selected AGN at z∼ 1 show little (or no) environmental dependencies within the same underlying population. We compare these results with a sample of local AGN drawn from the Sloan Digital Sky Survey (SDSS). Contrary to the high-redshift behaviour, we find that both LINERs and Seyferts in the SDSS show a slowly declining red sequence AGN fraction towards high-density environments. Interestingly, at z∼ 1 red sequence Seyferts and LINERs are approximately equally abundant. By z∼ 0, however, the red Seyfert population has declined relative to the LINER population by over a factor of ∼4.5. We speculate on possible interpretations of our results.

10.1111/j.1365-2966.2008.13893.x

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Citations (21)

A steep slope and small scatter for the high-mass end of the L–σ relation atz∼ 0.55

Monthly Notices of the Royal Astronomical Society (2016)

Antonio D. Montero-Dorta Yiping Shu A. Bolton Joel R. Brownstein Benjamin J. Weiner

We measure the intrinsic relation between velocity dispersion (σ) and luminosity (L) for massive, luminous red galaxies at redshift z ∼ 0.55. We achieve unprecedented precision by using a sample of 600 000 galaxies with spectra from the Baryon Oscillation Spectroscopic Survey of the third Sloan Digital Sky Survey (SDSS-III), covering a range of stellar masses M* ≳ 1011 M⊙. We deconvolve the effects of photometric errors, limited spectroscopic signal-to-noise ratio, and red–blue galaxy confusion using a novel hierarchical Bayesian formalism that is generally applicable to any combination of photometric and spectroscopic observables. For an L–σ relation of the form L ∝ σβ, we find β = 7.8 ± 1.1 for σ corrected to the effective radius, and a very small intrinsic scatter of s = 0.047 ± 0.004 in log10σ at fixed L. No significant redshift evolution is found for these parameters. The evolution of the zero-point within the redshift range considered is consistent with the passive evolution of a galaxy population that formed at redshift z = 2–3, assuming single stellar populations. An analysis of previously reported results seems to indicate that the passively evolved high-mass L–σ relation at z ∼ 0.55 is consistent with the one measured at z = 0.1. Our results, in combination with those presented in the LF work of Montero-Dorta et al., provide a detailed description of the high-mass end of the red sequence (RS) at z ∼ 0.55. This characterization, in the light of previous literature, suggest that the high-mass RS distribution corresponds to the 'core' elliptical population.

Stellar mass

Effective radius

Velocity dispersion

Stellar population

Photometric redshift

10.1093/mnras/stv2871

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Citations (16)

The SDSS DR6 luminosity functions of galaxies

Monthly Notices of the Royal Astronomical Society (2009)

Antonio D. Montero-Dorta Francisco Prada

We present number counts, luminosity functions (LFs) and luminosity densities of galaxies obtained using the Sloan Digital Sky Survey Sixth Data Release in all SDSS photometric bands. Thanks to the SDSS DR6, galaxy statistics have increased by a factor of ~9 in the u-band and by a factor of ~4-5 in the rest of the SDSS bands with respect to the previous work of Blanton et al. (2003b). In addition, we have achieved a high redshift completeness in our galaxy samples. Firstly, by making use of the survey masks, provided by the NYU-VAGC DR6, we have been able to define an area on the sky of high angular redshift completeness. Secondly, we guarantee that brightness-dependent redshift incompleteness is small within the magnitude ranges that define our galaxy samples. With these advances, we have estimated very accurate SDSS DR6 LFs in both the bright and the faint end. In the {0.1}^r-band, our SDSS DR6 luminosity function is well fitted by a Schechter LF with parameters Phi_{*}=0.90 +/- 0.07$, M_{*}-5log_{10}h=-20.73 +/- 0.04 and alpha=-1.23 +/- 0.02. As compared with previous results, we find some notable differences. In the bright end of the {0.1}^u-band luminosity function we find a remarkable excess, of ~1.7 dex at M_{{0.1}^u}=-20.5, with respect to the best-fit Schechter LF. This excess weakens in the {0.1}^g-band, fading away towards the very red {0.1}^z-band. A preliminary analysis on the nature of this bright-end bump reveals that it is mostly comprised of active galaxies and QSOs. It seems, therefore, that an important fraction of this exceeding luminosity may come from nuclear activity. In the faint end of the SDSS DR6 luminosity functions, where we can reach 1-1.5 magnitudes deeper than the previous SDSS LF estimation, we obtain a steeper slope [ABRIDGED].

Stellar mass

10.1111/j.1365-2966.2009.15197.x

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Citations (157)

How much dark matter is there inside early-type galaxies?★

Monthly Notices of the Royal Astronomical Society (2014)

A. Nigoche-Netro A. Ruelas-Mayorga P. Lagos G. Ramos-Larios C. Kehrig

We study the luminous mass as a function of the dynamical mass inside the effective radius (re) of early-type galaxies (ETGs) to search for differences between these masses. We assume Newtonian dynamics and that any difference between these masses is due to the presence of dark matter. We use several samples of ETGs – ranging from 19 000 to 98 000 objects – from the ninth data release of the Sloan Digital Sky Survey. We perform Monte Carlo (MC) simulations (see Appendix A) of galaxy samples and compare them with real samples. The main results are (i) MC simulations show that the distribution of the dynamical versus luminous mass depends on the mass range where the ETGs are distributed (geometric effect). This dependence is caused by selection effects and intrinsic properties of the ETGs. (ii) The amount of dark matter inside re is approximately 7 ± 22 per cent. (iii) This amount of dark matter is lower than the minimum estimate (10 per cent) found in the literature and four times lower than the average (30 per cent) of literature estimates. However, if we consider the associated error, our estimate is of the order of the literature average.

10.1093/mnras/stu2045

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Citations (8)