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Добірка наукової літератури з теми "Redshift Space"

Автор: Grafiati
Опубліковано: 1 квітня 2023

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Статті в журналах з теми "Redshift Space"

1

van den Busch, J. L., H. Hildebrandt, A. H. Wright, C. B. Morrison, C. Blake, B. Joachimi, T. Erben, C. Heymans, K. Kuijken, and E. N. Taylor. "Testing KiDS cross-correlation redshifts with simulations." Astronomy & Astrophysics 642 (October 2020): A200. http://dx.doi.org/10.1051/0004-6361/202038835.

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Анотація:
Measuring cosmic shear in wide-field imaging surveys requires accurate knowledge of the redshift distribution of all sources. The clustering-redshift technique exploits the angular cross-correlation of a target galaxy sample with unknown redshifts and a reference sample with known redshifts. It represents an attractive alternative to colour-based methods of redshift calibration. Here we test the performance of such clustering redshift measurements using mock catalogues that resemble the Kilo-Degree Survey (KiDS). These mocks are created from the MICE simulation and closely mimic the properties of the KiDS source sample and the overlapping spectroscopic reference samples. We quantify the performance of the clustering redshifts by comparing the cross-correlation results with the true redshift distributions in each of the five KiDS photometric redshift bins. Such a comparison to an informative model is necessary due to the incompleteness of the reference samples at high redshifts. Clustering mean redshifts are unbiased at |Δz|< 0.006 under these conditions. The redshift evolution of the galaxy bias of the reference and target samples represents one of the most important systematic errors when estimating clustering redshifts. It can be reliably mitigated at this level of precision using auto-correlation measurements and self-consistency relations, and will not become a dominant source of systematic error until the arrival of Stage-IV cosmic shear surveys. Using redshift distributions from a direct colour-based estimate instead of the true redshift distributions as a model for comparison with the clustering redshifts increases the biases in the mean to up to |Δz|∼0.04. This indicates that the interpretation of clustering redshifts in real-world applications will require more sophisticated (parameterised) models of the redshift distribution in the future. If such better models are available, the clustering-redshift technique promises to be a highly complementary alternative to other methods of redshift calibration.
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2

Percival, Will J., Lado Samushia, Ashley J. Ross, Charles Shapiro, and Alvise Raccanelli. "Redshift-space distortions." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 369, no. 1957 (December 28, 2011): 5058–67. http://dx.doi.org/10.1098/rsta.2011.0370.

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Comparing measurements of redshift-space distortions (RSDs) with geometrical observations of the expansion of the Universe offers tremendous potential for testing general relativity on very large scales. The basic linear theory of RSDs in the distant-observer limit has been known for 25 years and the effect has been conclusively observed in numerous galaxy surveys. The next generation of galaxy survey will observe many millions of galaxies over volumes of many tens of Gpc 3 . They will provide RSD measurements of such exquisite precision that we will have to carefully analyse and correct for many systematic deviations from this simple picture in order to fully exploit the statistical precision obtained. We review RSD theory and show how ubiquitous RSDs actually are, and then consider a number of potential systematic effects, shamelessly highlighting recent work in which we have been involved. This review ends by looking ahead to the future surveys that will make the next generation of RSD measurements.
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3

Ruggeri, Rossana, Will J. Percival, Héctor Gil-Marín, Fangzhou Zhu, Gong-Bo Zhao, and Yuting Wang. "Optimal redshift weighting for redshift-space distortions." Monthly Notices of the Royal Astronomical Society 464, no. 3 (September 23, 2016): 2698–707. http://dx.doi.org/10.1093/mnras/stw2422.

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4

Turner, Ross J., Guillaume Drouart, Nick Seymour, and Stanislav S. Shabala. "RAiSERed: radio continuum redshifts for lobed active galactic nuclei." Monthly Notices of the Royal Astronomical Society 499, no. 3 (October 6, 2020): 3660–72. http://dx.doi.org/10.1093/mnras/staa3067.

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ABSTRACT Next-generation radio surveys are expected to detect tens of millions of active galactic nuclei (AGNs) with a median redshift of $z$ ≥ 1. Beyond targeted surveys, the vast majority of these objects will not have spectroscopic redshifts, while photometric redshifts for high-redshift AGNs are of limited quality, and even then require optical and infrared photometry. We propose a new approach to measure the redshifts of lobed radio galaxies based exclusively on radio-frequency imaging and broad-band radio photometry. Specifically, our algorithm uses the lobe flux density, angular size and width, and spectral shape to derive probability density functions for the most likely source redshift based on the Radio AGN in Semi-analytic Environments dynamical model. The full physically based model explains 70 per cent of the variation in the spectroscopic redshifts of a high-redshift (2 &lt; $z$ &lt; 4) sample of radio AGNs, compared to at most 27 per cent for any one of the observed attributes in isolation. We find that upper bounds on the angular size, as expected for unresolved sources, are sufficient to yield accurate redshift measurements at $z$ ≥ 2. The error in the model upon calibration using at least nine sources with known spectroscopic redshifts is &lt;14 per cent in redshift (as 1 + $z$) across all redshifts. We provide the python code for the calculation and calibration of our radio continuum redshifts in an online library.
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Shepherd, C. W., R. G. Carlberg, H. K. C. Yee, and E. Ellingson. "The Real Space and Redshift Space Correlation Functions at Redshiftz= 1/3." Astrophysical Journal 479, no. 1 (April 10, 1997): 82–89. http://dx.doi.org/10.1086/303846.

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6

García-Farieta, Jorge Enrique, Federico Marulli, Alfonso Veropalumbo, Lauro Moscardini, Rigoberto A. Casas-Miranda, Carlo Giocoli, and Marco Baldi. "Clustering and redshift-space distortions in modified gravity models with massive neutrinos." Monthly Notices of the Royal Astronomical Society 488, no. 2 (July 8, 2019): 1987–2000. http://dx.doi.org/10.1093/mnras/stz1850.

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Abstract Modified gravity and massive neutrino cosmologies are two of the most interesting scenarios that have been recently explored to account for possible observational deviations from the concordance Λ cold dark matter (ΛCDM) model. In this context, we investigated the large-scale structure of the Universe by exploiting the dustgrain-pathfinder simulations that implement, simultaneously, the effects of f(R) gravity and massive neutrinos. To study the possibility of breaking the degeneracy between these two effects, we analysed the redshift-space distortions in the clustering of dark matter haloes at different redshifts. Specifically, we focused on the monopole and quadrupole of the two-point correlation function, both in real and redshift space. The deviations with respect to ΛCDM model have been quantified in terms of the linear growth rate parameter. We found that redshift-space distortions provide a powerful probe to discriminate between ΛCDM and modified gravity models, especially at high redshifts (z ≳ 1), even in the presence of massive neutrinos.
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7

Brisbin, Drew, Oskari Miettinen, Manuel Aravena, Vernesa Smolčić, Ivan Delvecchio, Chunyan Jiang, Benjamin Magnelli, et al. "An ALMA survey of submillimeter galaxies in the COSMOS field: Multiwavelength counterparts and redshift distribution." Astronomy & Astrophysics 608 (November 29, 2017): A15. http://dx.doi.org/10.1051/0004-6361/201730558.

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Анотація:
We carried out targeted ALMA observations of 129 fields in the COSMOS region at 1.25 mm, detecting 152 galaxies at S/N ≥ 5 with an average continuum RMS of 150 μJy. These fields represent a S/N-limited sample of AzTEC/ASTE sources with 1.1 mm S/N ≥ 4 over an area of 0.72 square degrees. Given ALMA’s fine resolution and the exceptional spectroscopic and multiwavelength photometric data available in COSMOS, this survey allows us unprecedented power in identifying submillimeter galaxy counterparts and determining their redshifts through spectroscopic or photometric means. In addition to 30 sources with prior spectroscopic redshifts, we identified redshifts for 113 galaxies through photometric methods and an additional nine sources with lower limits, which allowed a statistically robust determination of the redshift distribution. We have resolved 33 AzTEC sources into multi-component systems and our redshifts suggest that nine are likely to be physically associated. Our overall redshift distribution peaks at z ~ 2.0 with a high-redshift tail skewing the median redshift to \hbox{$\tilde{z}=2$}.48 ± 0.05. We find that brighter millimeter sources are preferentially found at higher redshifts. Our faintestsources, with S1.25 mm < 1.25 mJy, have a median redshift of \hbox{$\tilde{z}=2$}.18 ± 0.09, while the brightest sources, S1.25 mm > 1.8 mJy, have a median redshift of \hbox{$\tilde{z}=3$}.08 ± 0.17. After accounting for spectral energy distribution shape and selection effects, these results are consistent with several previous submillimeter galaxy surveys, and moreover, support the conclusion that the submillimeter galaxy redshift distribution is sensitive to survey depth.
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Sandhu, Gurcharn S. "Distinct Doppler Effects for Spontaneously Emitted Photons and Continuously Emitted Waves." Applied Physics Research 9, no. 4 (July 26, 2017): 44. http://dx.doi.org/10.5539/apr.v9n4p44.

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In this paper, we distinguish between the Doppler effects for spontaneously emitted photons and continuously emitted waves. Under certain plausible assumptions, electron orbits can be modeled for simple atomic systems and such studies show that all permissible electron trajectories correspond to elliptical orbits. From the conservation of energy, momentum and angular momentum, in conjunction with the geometrical model of electron orbits, we derive the Doppler effect for spontaneously emitted photons that is quite different from the one used for continuously generated waves. All astronomical redshifts are currently interpreted by assuming the incoming radiation to be continuously emitted waves. Therefore, widely-observed redshift in radiation from most astronomical sources is interpreted to imply the expanding universe, along with cosmological expansion of space. However, for the spontaneously emitted photons, we show that the photons emitted in forward direction parallel to the emitter velocity get redshifted. That means, the astronomical redshift implies that the emission sources are moving towards the observer and our universe is not expanding. All high redshift astronomical objects are likely to be physically disrupted through dynamic instabilities or explosions and their high redshifts are associated with relativistic shock waves propagating towards the observer. Hence the proposed Doppler effect for the spontaneously emitted photons dismisses the cosmological expansion of space and supports a steady state universe.
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Sicilian, Dominic, Francesca Civano, Nico Cappelluti, Johannes Buchner, and Alessandro Peca. "X-Ray Redshifts of Obscured Chandra Source Catalog Active Galactic Nuclei." Astrophysical Journal 936, no. 1 (August 29, 2022): 39. http://dx.doi.org/10.3847/1538-4357/ac82f4.

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Abstract We have computed obscured active galactic nuclei (AGN) redshifts using the XZ method, adopting a broad treatment in which we employed a wide-ranging data set and worked primarily at the XZ counts sensitivity threshold, culminating with a redshift catalog containing 121 sources that lack documented redshifts. We considered 363 obscured AGN from the Chandra Source Catalog Release 2.0, 59 of which were selected using multiwavelength criteria while 304 were X-ray selected. One third of the data set had crossmatched spectroscopic or photometric redshifts. These sources, dominated by low-z and low-N H AGN, were supplemented by 1000 simulations to form a data set for testing the XZ method. We used a multilayer perceptron neural network to examine and predict cases in which XZ fails to reproduce the known redshift, yielding a classifier that can identify and discard poor redshift estimates. This classifier demonstrated a statistically significant ∼3σ improvement over the existing XZ redshift information gain filter. We applied the machine-learning model to sources with no documented redshifts, resulting in the 121 source new redshift catalog, all of which were X-ray selected. Our neural network’s performance suggests that nearly 90% of these redshift estimates are consistent with hypothetical spectroscopic or photometric measurements, strengthening the notion that redshifts can be reliably estimated using only X-rays, which is valuable to current and future missions such as Athena. We have also identified a possible Compton-thick candidate that warrants further investigation.
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Fauber, Leah, Ming-Feng Ho, Simeon Bird, Christian R. Shelton, Roman Garnett, and Ishita Korde. "Automated measurement of quasar redshift with a Gaussian process." Monthly Notices of the Royal Astronomical Society 498, no. 4 (September 18, 2020): 5227–39. http://dx.doi.org/10.1093/mnras/staa2826.

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ABSTRACT We develop an automated technique to measure quasar redshifts in the Baryon Oscillation Spectroscopic Survey of the Sloan Digital Sky Survey (SDSS). Our technique is an extension of an earlier Gaussian process method for detecting damped Lyman α absorbers (DLAs) in quasar spectra with known redshifts. We apply this technique to a subsample of SDSS DR12 with BAL quasars removed and redshift larger than 2.15. We show that we are broadly competitive to existing quasar redshift estimators, disagreeing with the PCA redshift by more than 0.5 in only $0.38{{\ \rm per\ cent}}$ of spectra. Our method produces a probabilistic density function for the quasar redshift, allowing quasar redshift uncertainty to be propagated to downstream users. We apply this method to detecting DLAs, accounting in a Bayesian fashion for redshift uncertainty. Compared to our earlier method with a known quasar redshift, we have a moderate decrease in our ability to detect DLAs, predominantly in the noisiest spectra. The area under curve drops from 0.96 to 0.91. Our code is publicly available.
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Дисертації з теми "Redshift Space"

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McElroy, Kaitlin Marie, and Kaitlin Marie McElroy. "Modeling Redshift Space Distortions." Thesis, The University of Arizona, 2017. http://hdl.handle.net/10150/625092.

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PEZZOTTA, ANDREA. "Cosmological measurements and models of galaxy clustering and redshift-space distortions from galaxy redshift surveys." Doctoral thesis, Università degli Studi di Milano-Bicocca, 2017. http://hdl.handle.net/10281/158130.

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Анотація:
L'analisi congiunta di supernove Ia e delle anisotropie caratterizzanti la radiazione cosmica di fondo hanno evidenziato come l'Universo sia dominato da un'energia oscura capace di produrre l'espansione accelerata dello stesso. Questo scenario è degenere con la ben più radicale ipotesi che la Relatività Generale non sia più valida su scale cosmologiche; infatti, per una precisa scelta dei parametri, le teorie di gravità modificata sono in grado di predire la stessa espansione H(z) di un LCDM (energia oscura + GR) Questa degenerazione può essere rimossa misurando il tasso di crescita delle strutture, $f(z)$. Uno dei metodi migliori per misurare questo tasso è quello delle distorsioni nello spazio dei redshift (RSD). Quest'ultime compaiono quando i redshift misurati sono usati come indicatori di distanza, dato che essi contengono anche il contributo dato dalle velocità peculiari delle galassie, che è massimale lungo la linea di vista e dunque introduce delle anisotropie nel clustering misurato. Queste distorsioni nella, e.g, funzione di correlazione a due punti sono proporzionali al tasso di crescita. Nel dettaglio, se la Relatività Generale è valida anche su scale cosmologiche, allora ci si aspetta $f(z)\sim\Omega_m(z)]^{0.55}$; in caso contrario sono attese forme funzionali differenti. Purtroppo ottenere informazioni dalle survey di galassie non è semplice, in quanto la maggiorparte del segnale distorto è racchiuso all'interno di scale non lineari. Questo rende la modellizzazione del clustering non lineare uno dei punti cruciali della cosmologia moderna. Lo scopo finale del mio lavoro è stato la misura del tasso di crescita utilizzando i dati finali raccolti dalla survey VIPERS. Questa ha raccolto circa 100000 redshift all'interno di un lunghissimo intervallo di distanze, $0.4Observations of Type Ia Supernovae combined with the anisotropies of the Cosmic Microwave Background have reinforced the conclusion that the bulk of the total energy density contained in the Universe is dominated by a repulsive dark energy capable of driving the observed accelerated expansion. Unfortunately this scenario is highly degenerate with the more radical breakdown of General Relativity on cosmological scales; in this case, for a precise choice of parameters, modified gravity is able to predict the same expansion history H(z) as in a LCDM (dark energy + GR). In principle, this degeneracy can be lifted by measuring the growth rate of structure, which depends on the specific theory describing gravity. One of the most reliable probes of the growth of structures is provided by redshift-space distortions (RSD). These arise when measured redshifts are used as distance proxy since they contain also the contribution of galaxy peculiar velocities, that is maximal along the line of sight and thus introduces an anisotropy in the measured clustering. Such anisotropy in, e.g., the two-point correlation function, is proportional to the growth rate of cosmic structure f(z), which is a trademark of the gravity theory: if GR holds, we expect to measure a growth rate $f(z)\sim \Omega_m(z)]^{0.55}$; otherwise different forms are predicted. Unfortunately, extracting the linear RSD signal from galaxy redshift surveys is non-trivial, because much of the RSD signal lies on quasi-linear and non-linear scales. This requires a strong effort to properly model non-linear clustering and velocities. The final goal of my thesis project has been the measurement of the growth rate of structure from the new data of the complete VIPERS survey. VIPERS has used the VIMOS spectrograph at the ESO VLT to measure about 100000 galaxy redshifts over an extended redshift range, $0.4
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3

Warren, Stephen John. "The space density of optically-selected high-redshift quasars." Thesis, University of Cambridge, 1988. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.280032.

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Mountrichas, Georgios. "QSOs and galaxies : lensing, clustering and redshift-space distortions." Thesis, Durham University, 2008. http://etheses.dur.ac.uk/2246/.

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Анотація:
The aim of this thesis is to analyze statistically the available QSO, LRG, galaxy and cluster samples in order to estimate the QSO-galaxy lensing anti-correlation signal and measure the mass of foreground galaxies and clusters and to estimate the QSO-LRG clustering amplitude, the QSO bias and their dependence on QSO luminosity. We also investigate the behaviour of the group-galaxy infall parameter and their rms velocity dispersions for different group memberships. The aim here is to make dynamical estimates of the group masses to check the QSO lensing results. We first cross-correlate the SDSS photo-z, g < 21, 1.0 < Z(_p) < 2.2 QSOs with g < 21 galaxies and clusters in the same areas. The anti-correlation found is somewhat less than the results of Myers et al. based on 2QZ QSOs. But contamination of the QSOs by low redshift NELGs and QSOs can cause underestimation of the anticorrelation lensing signal. Correcting for such low redshift contamination at the levels indicated by our spectroscopic checks suggests that the effect is generally small for QSO cross-correlations with g < 21 galaxies but may be an issue for fainter galaxy samples. Thus when this correction is applied to the photo-z QSO sample of Scranton et al. the anti-correlation increases and the agreement with the 2QZ results of Myers et al. is improved. When we also take into account the fainter r < 21 galaxy limit of Scranton et al. as opposed to g < 21 for Myers et al., the two observational results appear to be in very good agreement. We then measure the bias of QSOs as a function of QSO luminosity at fixed redshift (z < 1) by cross-correlating them with Luminous Red Galaxies (LRGs) in the same spatial volume, hence breaking the degeneracy between QSO luminosity and redshift. We use three QSO samples from 2SLAQ, 2QZ and SDSS covering a QSO absolute magnitude range -24.5 < M(_bj) < -21.5, and cross-correlate them with 2SLAQ (z ≈ 0.5) and AAOmega (z ≈ 0.7) photometric and spectroscopic LRGs in the same redshift ranges. The 2-D and 3-D cross-clustering measurements are generally in good agreement. Our (2SLAQ) QSO-LRG clustering amplitude (r(_0) = 6.8 (^+0.1_-0.3)h(^-1)Mpc) as measured from the semi-projected cross-correlation function appears similar to the (2SLAQ) LRG-LRG auto-correlation amplitude (r(_0) = 7.45 ± 0.35h(^-1)Mpc) and both are higher than the (2QZ-t-2SLAQ) QSO-QSO amplitude (r(_0) ≈ 5.0h(^-1)Mpc). Our measurements show remarkably little QSO-LRG cross- clustering dependence on QSO luminosity. Assuming a standard ACDM model and values for b(_LRG) measured from LRG autocorrelation analyses, we find b(_Q) = 1.45 ± 0.11 at M(_bj) ≈ -24 and b(_Q) = 1.90 ± 0.16 at M(_bj) ≈ -22. We also find consistent results for the QSO bias from a z-space distortion analysis of the QSO-LRG cross-clustering at z ≈ 0.55. The velocity dispersions fitted to QSO-LRG cross-correlation, ع (σ,π), at 680 kms(^-1) are intermediate between those for QSO-QSO and LRG-LRG clustering, as expected given the larger QSO redshift errors. The dynamical infall results give ẞ(_Q) = 0.55 ± 0.10, implying b(_Q) = 1.4 ± 0.2. Thus both the z-space distortion and the amplitude analyses yield b(_Q) ≈ 1.5 at M(_bj) ≈ -23. The implied dark matter halo mass inhabited by QSOs at z ≈ 0.55 is ~ 10(^13)h(^-1)M(_ʘ), again approximately independent of QSO luminosity. Prompted by the indications from QSO lensing that there may be more mass associated with galaxy groups than expected from virial analyses, we make new dynamical infall estimates of the masses associated with 2PIGG groups and clusters. We analyse the redshift distortions in the cluster-galaxy cross-correlation function as a function of cluster membership, cross-correlating z < 0.12 2PIGG clusters and groups with the full 2dF galaxy catalogue. We make estimates of the dynamical infall parameter, ẞ, and new estimates of the group velocity dispersions for group membership classes out to z < 0.12. We first find that, out to 30-40h(^-1)Mpc, the amplitude of the full 3-D redshift space cross-correlation function, ع (_cg), rises monotonically with group membership. We use a simple linear-theory infall model to fit ع (σ,π), in the range 5 < s < 40h(^-1) Mpc. We find that the ẞ versus membership relation for the data shows a minimum at intermediate group membership n ≈ 20 or L ≈ 2 x l0(^11)h(^-2)L(_ʘ), implying that the bias and hence M/L ratios rise by a significant factor (≈ 5x) both for small groups and rich clusters. The minimum for the mocks is at a 2 - 3x lower luminosity than for the data. However, the mocks also show a systematic shift between the location of the ẞ minimum and the M/L minimum at L ≈ l0(^11)h(^-2)L(_ʘ), given by direct calculation using the known DM distribution. Our overall conclusion is that bias estimates from dynamical infall appear to support the minimum in star-formation efficiency at intermediate halo masses. Nevertheless, there may still be significant systematic problems arising from measuring ẞ x (^1/_b) ∂P(_mass) /∂P(_gaiaxies) using large-scale infall rather than M/L using small-scale velocity dispersions
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5

Gouws, Liesbeth-Helena. "Redshift-space distortions as a probe of dark energy." Thesis, University of Western Cape, 2014. http://hdl.handle.net/11394/3342.

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Анотація:
>Magister Scientiae - MSc
We begin by finding a system of differential equations for the background and linearly perturbed variables in the standard, ɅCDM model, using the Einstein Field Equations, and then solving these numerically. Later, we extend this to dynamical dark energy models parameterised by an equation of state, w, and a rest frame speed of sound, cs. We pay special attention to the large-scale behaviour of Δm, the gauge invariant, commoving matter density, since the approximation Δm ≃ δm, where δm is the longitudinal gauge matter density, is more commonly used, but breaks down at large scales. We show how the background is affected by w only, so measurements of perturbations are required to constrain cs. We examine how the accelerated expansion of the universe, caused by dark energy, slows down the growth rate of matter. We then show the matter power spectrum is not in itself useful for constraining dark energy models, but how redshift-space distortions can be used to extract the growth rate from the galaxy power spectrum, and hence how redshift-space power spectra can be used to constrain different dark energy models. We find that on small scales, the growth rate is more dependent on w, while on large scales, it depends more on cs.
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Petracca, Fernanda <1983&gt. "Constraints on neutrino mass fraction using Redshift Space Distortions." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2014. http://amsdottorato.unibo.it/6728/1/Fernanda_Petracca_tesi.pdf.

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Анотація:
Redshift Space Distortions (RSD) are an apparent anisotropy in the distribution of galaxies due to their peculiar motion. These features are imprinted in the correlation function of galaxies, which describes how these structures distribute around each other. RSD can be represented by a distortions parameter $\beta$, which is strictly related to the growth of cosmic structures. For this reason, measurements of RSD can be exploited to give constraints on the cosmological parameters, such us for example the neutrino mass. Neutrinos are neutral subatomic particles that come with three flavours, the electron, the muon and the tau neutrino. Their mass differences can be measured in the oscillation experiments. Information on the absolute scale of neutrino mass can come from cosmology, since neutrinos leave a characteristic imprint on the large scale structure of the universe. The aim of this thesis is to provide constraints on the accuracy with which neutrino mass can be estimated when expoiting measurements of RSD. In particular we want to describe how the error on the neutrino mass estimate depends on three fundamental parameters of a galaxy redshift survey: the density of the catalogue, the bias of the sample considered and the volume observed. In doing this we make use of the BASICC Simulation from which we extract a series of dark matter halo catalogues, characterized by different value of bias, density and volume. This mock data are analysed via a Markov Chain Monte Carlo procedure, in order to estimate the neutrino mass fraction, using the software package CosmoMC, which has been conveniently modified. In this way we are able to extract a fitting formula describing our measurements, which can be used to forecast the precision reachable in future surveys like Euclid, using this kind of observations.
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Petracca, Fernanda <1983&gt. "Constraints on neutrino mass fraction using Redshift Space Distortions." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2014. http://amsdottorato.unibo.it/6728/.

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Анотація:
Redshift Space Distortions (RSD) are an apparent anisotropy in the distribution of galaxies due to their peculiar motion. These features are imprinted in the correlation function of galaxies, which describes how these structures distribute around each other. RSD can be represented by a distortions parameter $\beta$, which is strictly related to the growth of cosmic structures. For this reason, measurements of RSD can be exploited to give constraints on the cosmological parameters, such us for example the neutrino mass. Neutrinos are neutral subatomic particles that come with three flavours, the electron, the muon and the tau neutrino. Their mass differences can be measured in the oscillation experiments. Information on the absolute scale of neutrino mass can come from cosmology, since neutrinos leave a characteristic imprint on the large scale structure of the universe. The aim of this thesis is to provide constraints on the accuracy with which neutrino mass can be estimated when expoiting measurements of RSD. In particular we want to describe how the error on the neutrino mass estimate depends on three fundamental parameters of a galaxy redshift survey: the density of the catalogue, the bias of the sample considered and the volume observed. In doing this we make use of the BASICC Simulation from which we extract a series of dark matter halo catalogues, characterized by different value of bias, density and volume. This mock data are analysed via a Markov Chain Monte Carlo procedure, in order to estimate the neutrino mass fraction, using the software package CosmoMC, which has been conveniently modified. In this way we are able to extract a fitting formula describing our measurements, which can be used to forecast the precision reachable in future surveys like Euclid, using this kind of observations.
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8

Ishikawa, Takashi. "Systematic errors of cosmological gravity test using redshift space distortion." 京都大学 (Kyoto University), 2015. http://hdl.handle.net/2433/199104.

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9

Cruz, da Angela José Antonio. "Clustering and redshift-space distortions in QSO and galaxy surveys." Thesis, Durham University, 2006. http://etheses.dur.ac.uk/2342/.

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In this thesis, we exploit the potential of existing QSO and galaxy surveys for investigating the nature of the large scale structure in the Universe. A detailed analysis of clustering and redshift- space distortions allows us to constrain cosmological parameters. We model the anisotropies due to dynamical and geometrical effects in the measured clustering pattern of distant QSOs from the 2dF QSO Survey (2QZ) and also Lyman break galaxies. The 2QZ is then combined with the QSO sample from the 2dF SDSS LRG and QSO Survey (2SLAQ) to study the luminosity dependence of QSO clustering. Using AT-body simulations, we estimate the statistical gains in the determination of cosmological parameters from future LRG surveys. We measure the clustering of distant QSOs from the 2QZ survey by performing a correlation analysis of redshift-space (z-space) distortions. To interpret the z-space correlation function measured in orthogonal directions, ع(σ,π)， we require an accurate model for the QSO real-space correlation function, ع (r). Motivated by the form for ع (r) seen in the 2dF Galaxy Redshift Survey (2dFGRS) and in standard ACDM predictions, we use a double power-law model for ع (r). which gives a good fit to the z-space and projected correlation functions. By fitting functional forms of ع(σ,π) which include both dynamical and geometrical modelling, we find, as expected, that β (which parameterises the infall into overdense regions) and the density of the Universe (Ω(^0_M)) are degenerate. However, this degeneracy can be lifted by using linear theory predictions under different cosmological scenarios. Using the 2QZ survey, we obtain: βQAO (z=1.4) = 0.50 (^0.13_0.15), Ω(^0_M) = 0.35 (^+0.19_-0.13). The modelling of geometrical and dynamical anisotropies in the measured ع(σ,π) pattern is then applied to a sample of distant Lymari-break galaxies. The presence of feedback mechanisms in these z〜 3 star-forming galaxies heightens the importance of understanding the effects of z-space distortions. Despite the limited size of the fields, which hampers the determination of ع(r) at large scales, we find that a double-power law ع(s) parameterisation is consistent with the correlation function measurements. This double power law model is then used as an input for the ع(σ,π) fitting and subsequent constraining of cosmological parameters. This investigation reveals that: ßLBG (z= 3) = 0.25± (^+0.05_-0.05) and Ω(^0_M) = 0.55(^+0.45_-0.16). The combination of the 2QZ with the fainter 2SLAQ QSO sample reveals that QSO clustering does not depend strongly on luminosity. This result is consistent with models which predict that haloes of similar mass can harbour QSOs of different luminosities. By assuming ellipsoidal models for the collapse of density perturbations, we test this hypothesis and estimate the mass of the dark matter haloes which the QSOs inhabit. We find that halo mass does not seem to evolve strongly with redshift nor depend on QSO luminosity. Having determined the black hole mass associated with the QSOs, we investigate how it correlates with luminosity and redshift and ascertain the relation between Eddington efficiency and black hole mass. Our results suggest that: (i) black hole mass does not depend strongly on accretion efficiency and (іі) black holes associated with QSOs of different luminosities have similar masses. Finally, the Hubble Volume simulation is used to construct a mock sample of a future ΑΑΩ Luminous Red Galaxy (LRG) survey. The ultimate aims of this survey are to identify the baryon acoustic features in the LRG clustering signal and to determine the equation of state of dark energy. We apply the z-space distortion analysis developed previously in the thesis to infer the statistical gain in terms of determinations of ß(_LRG) (z~ 0.7) and Ω(+0_m) .This thesis exploits the wealth of information contained in cosmological surveys, and demonstrates how the use of tools such as clustering statistics or z-space distortion analyses permit the extraction of such information.
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Tansley, David. "ISO observations of dust in low redshift radio galaxies." Thesis, University of Bristol, 2000. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.324359.

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Книги з теми "Redshift Space"

1

Taylor, A. N. Non-linear cosmological power spectra in real and redshift space. [Washington, DC: National Aeronautics and Space Administration, 1996.

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Taylor, A. N. Non-linear cosmological power spectra in real and redshift space. [Washington, DC: National Aeronautics and Space Administration, 1996.

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3

Taylor, A. N. Non-linear cosmological power spectra in real and redshift space. [Washington, DC: National Aeronautics and Space Administration, 1996.

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4

Taylor, A. N. Non-linear cosmological power spectra in real and redshift space. [Washington, DC: National Aeronautics and Space Administration, 1996.

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5

Chris, Impey, and United States. National Aeronautics and Space Administration., eds. Ultraviolet spectropolarimetry of high redshift quasars with the Hubble Space Telescope. [Washington, DC: National Aeronautics and Space Administration, 1993.

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6

Herstmonceaux Conference (37th 1996 Cambridge). The Hubble space telescope and the high redshift universe: The 37th Herstmonceux conference, Cambridge, United Kingdom,July 1-5, 1996. Edited by Tanvir Nial R, Aragon-Salamanca Alfonso, and Wall Jasper V. Singapore: World Scientific, 1997.

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7

Herstmonceux Conference (37th 1996 Cambridge, England). The Hubble Space Telescope and the high redshift universe / 37th Herstmonceux Conference, Cambridge, United Kingdom, July 1-5, 1996 ; editors, Nial R. Tanvir, Alfonso Aragón-Salamanca, Jasper V. Wall. Singapore: World Scientific, 1997.

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8

Scalzi, John. Redshirts. Waterville, Maine: Thorndike Press, A part of Gale, Cengage Learning, 2015.

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9

Scalzi, John. Redshirts. New York: Tor, 2012.

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10

The Hubble Space Telescope and the High Redshift Universe: Proceedings of the 37th Herstmonceux Conference. World Scientific Publishing Company, 1997.

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Частини книг з теми "Redshift Space"

1

Fairall, A. P. "Southern Redshift Plots." In Astrophysics and Space Science Library, 343–44. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0903-8_35.

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2

Appenzeller, Immo. "The Space Distribution of High-redshift Galaxies." In High-Redshift Galaxies, 269–76. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-75824-2_8.

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3

Tucker, Douglas L. "The Las Campanas Redshift Survey Results: The Redshift-Space Autocorrelation Function." In Astrophysics and Space Science Library, 117–21. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-4960-0_11.

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4

Kaiser, Nick. "Clustering in Real Space vs Redshift Space." In Galaxy Distances and Deviations from Universal Expansion, 271–72. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4702-3_45.

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5

Lilje, Per B., and G. Efstathiou. "Correlation Functions in Redshift Space." In Astrophysics and Space Science Library, 393–94. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0903-8_60.

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6

Maddox, S. J., G. B. Dalton, G. Efstathiou, and W. J. Sutherland. "The APM Cluster Redshift Survey." In Astrophysics and Space Science Library, 313–21. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2472-0_41.

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7

Seitter, W. C. "The Muenster Redshift Project — MRSP." In Astrophysics and Space Science Library, 367–81. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2472-0_47.

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8

Bruzual, Gustavo. "Galaxy Morphology at Large Redshift." In Astrophysics and Space Science Library, 161–76. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2919-7_20.

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9

Gunn, James E., and Alan Dressier. "Cluster Galaxies at High Redshift." In Astrophysics and Space Science Library, 227–37. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2919-7_28.

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10

Hamilton, A. J. S. "Linear Redshift Distortions: A Review." In Astrophysics and Space Science Library, 185–275. Dordrecht: Springer Netherlands, 1998. http://dx.doi.org/10.1007/978-94-011-4960-0_17.

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Тези доповідей конференцій з теми "Redshift Space"

1

Marshall, Oriel, Rita Tojeiro, and Anne-Marie Weijmans. "Demonstrating cosmological and Doppler redshift in the classroom." In Symposium on Space Educational Activities (SSAE). Universitat Politècnica de Catalunya, 2022. http://dx.doi.org/10.5821/conference-9788419184405.098.

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Cosmology is often a difficult subject to teach as it can involve many confusing and sometimes abstract concepts. One particular topic with many existing misconceptions and difficulties surrounding it is redshift, specifically the difference between Doppler shift (due to the peculiar velocities of galaxies) and cosmological redshift (due to the expansion of the side). Redshift of galaxies, despite being an extremely useful and interesting scientific tool, can often become a tedious subject to teach as it is largely theoretical and usually does not include demonstrations or interaction in the classroom. It can be challenging to understand, and therefore also challenging to explain, the differences between Doppler and cosmological redshift, often leading to this distinction being overlooked entirely. The set of demonstrations developed during this astrophysics masters project, along with the accompanying presentation, worksheet, and teacher notes, aim to explain both Doppler and cosmological redshift clearly and in an engaging and memorable way. The demonstrations use remote control vehicles to represent peaks of a travelling wave of light. When demonstrating Doppler shift, the vehicles are released from a plastic board that is being pulled away, representing a receding source of light. When demonstrating cosmological redshift, the vehicles are driven along a wide stretchy exercise band, representing a section of the expanding Universe through which this wave of light is travelling. This teaching resource will introduce interactive learning, proven to be very effective when teaching astronomy, and provides a useful and fun physical analogy to demonstrate an often-misunderstood subject.
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2

Guzzo, Luigi, Olivier Le Fèvre, Jean-Michel Alimi, and André Fuözfa. "Redshift-space distortions in deep redshift surveys as a probe of the invisible Universe." In INVISIBLE UNIVERSE: Proceedings of the Conference. AIP, 2010. http://dx.doi.org/10.1063/1.3462662.

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3

Bowers, C., B. Woodgate, R. Kimble, M. Kaiser, S. Kraemer, T. Gull, S. Heap, et al. "Performance of the space telescope imaging spectrograph." In The ultraviolet universe at low and high redshift. AIP, 1997. http://dx.doi.org/10.1063/1.53814.

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4

Raccanelli, Alvise, Phil Bull, Stefano Camera, Chris Blake, Pedro Ferreira, Roy Maartens, Mario Santos, et al. "Measuring redshift-space distortion with future SKA surveys." In Advancing Astrophysics with the Square Kilometre Array. Trieste, Italy: Sissa Medialab, 2015. http://dx.doi.org/10.22323/1.215.0031.

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5

Smith, Eric P., John Mather, Pierre Bely, Anuradha Koratkar, Massino Stiavelli, and H. S. (Peter) Stockman. "The next generation space telescope design reference mission." In The ultraviolet universe at low and high redshift. AIP, 1997. http://dx.doi.org/10.1063/1.53770.

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Mather, John C., Eric P. Smith, Bernard D. Seery, Pierre Y. Bely, Massimo Stiavelli, H. S. Stockman, and Richard Burg. "Redshifted UV Astronomy with the next generation space telescope." In The ultraviolet universe at low and high redshift. AIP, 1997. http://dx.doi.org/10.1063/1.53813.

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7

Tanvir, Nial R., Alfonso AragÓn-Salamanca, and Jasper V. Wall. "THE HUBBLE SPACE TELESCOPE AND THE HIGH REDSHIFT UNIVERSE." In 37th Herstmonceux Conference. WORLD SCIENTIFIC, 1997. http://dx.doi.org/10.1142/9789814530408.

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8

MÜLLER, H., M. A. HOHENSEE, and N. YU. "MATTER-WAVE TESTS OF THE GRAVITATIONAL REDSHIFT IN SPACE." In Proceedings of the Fifth Meeting. WORLD SCIENTIFIC, 2010. http://dx.doi.org/10.1142/9789814327688_0002.

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9

Chabaud, Pierre-Yves, Maxime Leurent, and Christian Surace. "ARIADNE : a system for evaluation of AMAZED’s spectroscopic redshift estimation efficiency." In 15th International Conference on Space Operations. Reston, Virginia: American Institute of Aeronautics and Astronautics, 2018. http://dx.doi.org/10.2514/6.2018-2378.

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Schmidt, Maarten. "Luminosities, space densities and redshift distributions of gamma-ray bursts." In The fifth huntsville gamma-ray burst symposium. AIP, 2000. http://dx.doi.org/10.1063/1.1361507.

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Звіти організацій з теми "Redshift Space"

1

Yu, Weixiang, and Gordon T. Richards. LSSTC AGN Data Challenge 2021. GitHub, July 2021. http://dx.doi.org/10.17918/agn_datachallenge.

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We provide a code and data repository that can be used to facilitate planning for AGN science with the upcoming Vera C. Rubin Observatory's Legacy Survey of Space and Time (LSST). For this purpose, we have produced a common exploratory dataset that can be used to develop tools for parameterization of AGN light curves, AGN selection, and AGN photometric redshifts
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