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Journal articles on the topic 'Galaxy correlation'

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Published: 3 June 2025

Last updated: 20 July 2025

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1

Smith, Jr. Daniel M. "City-City Correlations to Introduce Galaxy-Galaxy Correlations." Communicating Astronomy with the Public Journal 8, no. 2 (2014): 31–34. https://doi.org/10.5281/zenodo.14928982.

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The large-scale structure of the Universe, vividly displayed by the spatial distribution of galaxies, is characterised quantitatively by the two-point galaxy–galaxy correlation function. But the meaning of the correlation function is somewhat abstract because it does not have a ready analogy. This work computes the two-dimensional, two-point city–city correlation function for three populous regions of the United States, demonstrating that the city–city correlation function is analogous to the galaxy–galaxy correlation function determined from Sloan Digital Sky Survey data. City radii are analogous to galaxy cluster radii, and city-to-city distances are analogous to distances between galaxy clusters. Part of this work has been adapted for a lab suitable for non-experts.

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Watts, Peter, and Peter Schneider. "Higher Order Cross-Correlation Functions from Galaxy-Galaxy-Galaxy Lensing." Proceedings of the International Astronomical Union 2004, IAUS225 (2004): 243–48. http://dx.doi.org/10.1017/s1743921305002048.

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Xu, Xiaoju, and Zheng Zheng. "Galaxy assembly bias of central galaxies in the Illustris simulation." Monthly Notices of the Royal Astronomical Society 492, no. 2 (2020): 2739–54. http://dx.doi.org/10.1093/mnras/staa009.

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ABSTRACT Galaxy assembly bias, the correlation between galaxy properties and halo properties at fixed halo mass, could be an important ingredient in halo-based modelling of galaxy clustering. We investigate the central galaxy assembly bias by studying the relation between various galaxy and halo properties in the Illustris hydrodynamic galaxy formation simulation. Galaxy stellar mass M* is found to have a tighter correlation with peak maximum halo circular velocity Vpeak than with halo mass Mh. Once the correlation with Vpeak is accounted for, M* has nearly no dependence on any other halo assembly variables. The correlations between galaxy properties related to star formation history and halo assembly properties also show a cleaner form as a function of Vpeak than as a function of Mh, with the main correlation being with halo formation time and to a less extent halo concentration. Based on the galaxy–halo relation, we present a simple model to relate the bias factors of a central galaxy sample and the corresponding halo sample, both selected based on assembly-related properties. It is found that they are connected by the correlation coefficient of the galaxy and halo properties used to define the two samples, which provides a reasonable description for the samples in the simulation and suggests a simple prescription to incorporate galaxy assembly bias into the halo model. By applying the model to the local galaxy clustering measurements in Lin et al., we infer that the correlation between star formation history or specific star formation rate and halo formation time is consistent with being weak.

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Newman, Andrew B., Mahdi Qezlou, Nima Chartab та ін. "LATIS: Constraints on the Galaxy–Halo Connection at z ∼ 2.5 from Galaxy–Galaxy and Galaxy–Lyα Clustering". Astrophysical Journal 961, № 1 (2024): 27. http://dx.doi.org/10.3847/1538-4357/ad0896.

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Abstract The connection between galaxies and dark matter halos is often quantified using the stellar mass–halo mass (SMHM) relation. Optical and near-infrared imaging surveys have led to a broadly consistent picture of the evolving SMHM relation based on measurements of galaxy abundances and angular correlation functions. Spectroscopic surveys at z ≳ 2 can also constrain the SMHM relation via the galaxy autocorrelation function and through the cross-correlation between galaxies and Lyα absorption measured in transverse sight lines; however, such studies are very few and have produced some unexpected or inconclusive results. We use ∼3000 spectra of z ∼ 2.5 galaxies from the Lyα Tomography IMACS Survey (LATIS) to measure the galaxy–galaxy and galaxy–Lyα correlation functions in four bins of stellar mass spanning 109.2 ≲ M */M ⊙ ≲ 1010.5. Parallel analyses of the MultiDark N-body and ASTRID hydrodynamic cosmological simulations allow us to model the correlation functions, estimate covariance matrices, and infer halo masses. We find that results of the two methods are mutually consistent and broadly accord with standard SMHM relations. This consistency demonstrates that we are able to measure and model Lyα transmission fluctuations δ F in LATIS accurately. We also show that the galaxy–Lyα cross-correlation, a free by-product of optical spectroscopic galaxy surveys at these redshifts, can constrain halo masses with similar precision to galaxy–galaxy clustering.

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Slosar, Anže, Kate Land, Steven Bamford, et al. "Galaxy Zoo: chiral correlation function of galaxy spins★." Monthly Notices of the Royal Astronomical Society 392, no. 3 (2009): 1225–32. http://dx.doi.org/10.1111/j.1365-2966.2008.14127.x.

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O’Donnell, Christine, Peter Behroozi, and Surhud More. "Observing correlations between dark matter accretion and galaxy growth – I. Recent star formation activity in isolated Milky Way-mass galaxies." Monthly Notices of the Royal Astronomical Society 501, no. 1 (2020): 1253–72. http://dx.doi.org/10.1093/mnras/staa3654.

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ABSTRACT The correlation between fresh gas accretion on to haloes and galaxy star formation is critical to understanding galaxy formation. Different theoretical models have predicted different correlation strengths between halo accretion rates and galaxy star formation rates, ranging from strong positive correlations to little or no correlation. Here, we present a technique to observationally measure this correlation strength for isolated Milky Way-mass galaxies with z &lt; 0.123. This technique is based on correlations between dark matter accretion rates and the projected density profile of neighbouring galaxies; these correlations also underlie past work with splashback radii. We apply our technique to both observed galaxies in the Sloan Digital Sky Survey as well as simulated galaxies in the UniverseMachine where we can test any desired correlation strength. We find that positive correlations between dark matter accretion and recent star formation activity are ruled out with $\gtrsim 85{{\ \rm per\ cent}}$ confidence. Our results suggest that star formation activity may not be correlated with fresh accretion for isolated Milky Way-mass galaxies at z = 0 and that other processes, such as gas recycling, dominate further galaxy growth.

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Merchan, Manuel E., Marcio A. G. Maia, and Diego G. Lambas. "Correlation Function of Galaxy Groups." Astrophysical Journal 545, no. 1 (2000): 26–31. http://dx.doi.org/10.1086/317772.

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Ghosh অরিত্র, Aritra ঘোষ, C. Megan Urry, Meredith C. Powell, et al. "Denser Environments Cultivate Larger Galaxies: A Comprehensive Study beyond the Local Universe with 3 Million Hyper Suprime-Cam Galaxies." Astrophysical Journal 971, no. 2 (2024): 142. http://dx.doi.org/10.3847/1538-4357/ad596f.

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Abstract The relationship between galaxy size and environment has remained enigmatic, with over a decade of conflicting results. We present one of the first comprehensive studies of the variation of galaxy radius with environment beyond the local Universe and demonstrate that large-scale environmental density is correlated with galaxy radius independent of stellar mass and galaxy morphology. We confirm with >5σ confidence that galaxies in denser environments are up to ∼25% larger than their equally massive counterparts with similar morphology in less dense regions of the Universe. We achieve this result by correlating projected two-dimensional densities over ∼360 deg2 with the structural parameters of ∼3 million Hyper Suprime-Cam galaxies at 0.3 ≤ z < 0.7 with log M / M ⊙ ≥ 8.9 . Compared to most previous studies, this sample is ∼100–10,000 times larger and goes ∼1 dex deeper in mass completeness. We demonstrate that past conflicting results have been driven by small sample sizes and a lack of robust measurement uncertainties. We verify the presence of the above correlation separately for disk-dominated, bulge-dominated, star-forming, and quiescent subpopulations. We find the strength of the correlation to be dependent on redshift, stellar mass, and morphology. The correlation is strongest at lower redshifts and systematically weakens or disappears beyond z ≥ 0.5. At z ≥ 0.5, more massive galaxies still display a statistically significant correlation. Although some existing theoretical frameworks can be selectively invoked to explain some of the observed correlations, our work demonstrates the need for more comprehensive theoretical investigations of the correlation between galaxy size and environment.

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9

Kerscher, Martin. "Spatial range of conformity." Astronomy & Astrophysics 615 (July 2018): A109. http://dx.doi.org/10.1051/0004-6361/201731212.

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Context. Properties of galaxies, such as their absolute magnitude and stellar mass content, are correlated. These correlations are tighter for close pairs of galaxies, which is called galactic conformity. In hierarchical structure formation scenarios, galaxies form within dark matter haloes. To explain the amplitude and spatial range of galactic conformity two-halo terms or assembly bias become important. Aims. With the scale dependent correlation coefficients, the amplitude and spatial range of conformity are determined from galaxy and halo samples. Methods. The scale dependent correlation coefficients are introduced as a new descriptive statistic to quantify the correlations between properties of galaxies or haloes, depending on the distances to other galaxies or haloes. These scale dependent correlation coefficients can be applied to the galaxy distribution directly. Neither a splitting of the sample into subsamples, nor an a priori clustering is needed. Results. This new descriptive statistic is applied to galaxy catalogues derived from the Sloan Digital Sky Survey III and to halo catalogues from the MultiDark simulations. In the galaxy sample the correlations between absolute magnitude, velocity dispersion, ellipticity, and stellar mass content are investigated. The correlations of mass, spin, and ellipticity are explored in the halo samples. Both for galaxies and haloes a scale dependent conformity is confirmed. Moreover the scale dependent correlation coefficients reveal a signal of conformity out to 40 Mpc and beyond. The halo and galaxy samples show a differing amplitude and range of conformity.

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Gaztanaga, E. "High-order galaxy correlation functions in the APM Galaxy Survey." Monthly Notices of the Royal Astronomical Society 268, no. 4 (1994): 913–24. http://dx.doi.org/10.1093/mnras/268.4.913.

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Croton, D. J., E. Gaztañaga, C. M. Baugh, et al. "The 2dF Galaxy Redshift Survey: higher-order galaxy correlation functions." Monthly Notices of the Royal Astronomical Society 352, no. 4 (2004): 1232–44. http://dx.doi.org/10.1111/j.1365-2966.2004.08017.x.

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Jing Yi-Ping and Zhang Jia-lü. "Cosmic strings and the two-point galaxy-galaxy correlation function." Chinese Astronomy and Astrophysics 12, no. 2 (1988): 159–63. http://dx.doi.org/10.1016/0275-1062(88)90012-4.

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Linke, Laila, Patrick Simon, Peter Schneider, and Stefan Hilbert. "Measuring galaxy-galaxy-galaxy-lensing with higher precision and accuracy." Astronomy & Astrophysics 634 (January 29, 2020): A13. http://dx.doi.org/10.1051/0004-6361/201936693.

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Context. Galaxy-galaxy-galaxy lensing (G3L) is a powerful tool for constraining the three-point correlation between the galaxy and matter distribution and thereby models of galaxy evolution. Aims. We propose three improvements to current measurements of G3L: (i) a weighting of lens galaxies according to their redshift difference, (ii) adaptive binning of the three-point correlation function, and (iii) accounting for the effect of lens magnification by the cosmic large-scale structure. Improvement (i) is designed to improve the precision of the G3L measurement, whereas improvements (ii) and (iii) remove biases of the estimator. We further show how the G3L signal can be converted from angular into physical scales. Methods. The improvements were tested on simple mock data and simulated data based on the Millennium Run with an implemented semi-analytic galaxy model. Results. Our improvements increase the signal-to-noise ratio by 35% on average at angular scales between 0.′1 and 10′ and physical scales between 0.02 and 2 h−1 Mpc. They also remove the bias of the G3L estimator at angular scales below 1′, which was originally up to 40%. The signal due to lens magnification is approximately 10% of the total signal.

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Hu Yang, X., H. J. Mo, G. Kauffmann, and Y. Q. Chu. "Understanding the results of galaxy-galaxy lensing using galaxy-mass correlation in numerical simulations." Monthly Notices of the Royal Astronomical Society 339, no. 2 (2003): 387–96. http://dx.doi.org/10.1046/j.1365-8711.2003.06217.x.

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Pereira, Marco. "Testing the Correlation Between Host Galaxy Mass and Redshift Using the Pantheon Survey Data." Engineering and Applied Sciences Journal 2, no. 2 (2025): 01–03. https://doi.org/10.64030/3067-8005.02.02.01.

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This study investigates the relationship between redshift and host galaxy mass using the Pantheon Supernova Survey dataset. The hypothesis that galaxies with identical luminous distances should have the same host mass is tested using statistical correlation analysis. Contrary to expectations from contraction-based cosmological models, our findings indicate. • No statistically significant correlation between redshift and host galaxy mass. • A very strong correlation (r = 0.979) between redshift and photometric distance derived from Type IA Supernovae. • The complete absence of evidence supporting gravitational red shifting as a dominant factor in cosmological redshifts. Furthermore, we identify critical methodological flaws in João Barcellos’ previous analysis, which used only 50 galaxies, ignored the Pantheon dataset, and discarded numerical information in favor of an arbitrary binary classification. Our results support the standard interpretation of redshift as a distance measure rather than an effect of host galaxy mass.

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Croom, Scott M. "QSO-Galaxy Correlations: Lensing or Dust?" Publications of the Astronomical Society of Australia 18, no. 2 (2001): 169–71. http://dx.doi.org/10.1071/as01012.

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AbstractWe present evidence for an anti-correlation between faint QSOs and B < 23 galaxies.A sample of 192 QSOs in a 2.5 deg2 area has been imaged using the Isaac Newton Telescope Wide-Field Camera. The cross-correlation signal is of a similar amplitude to the galaxy auto-correlation function at the limit of B < 23, but is negative in sign. As fainter galaxies are selected the negative correlation signal becomes less significant, until the signal is effectively zero at B < 26. We propose two alternate explanations for the observed effect. The first is gravitational lensing of the faint background QSOs, which have a flat number count slope. However, the lensing signal is significantly higher than expected in conventional models. The second possibility is that inter-galactic dust absorption is responsible. A reddening of only E(B - V) ≃ 0.02 is required to produce the observed correlation. The large 2dF and SDSS QSO surveys should allow a definitive solution to the question of QSO–galaxy correlations.

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Wirén, S., M. J. Valtonen, and B. Liu. "Binary Galaxy Spin Correlations in Small Galaxy Groups." International Astronomical Union Colloquium 174 (2000): 296–98. http://dx.doi.org/10.1017/s0252921100055159.

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AbstractStatistics of spin orientations in binary galaxies may be used as a tool to study the formation process of galaxies. Helou (1984) found that the spins of spiral galaxies in binary systems are anticorrelated, and he suggested that it may have to do with the inclination dependence of the galaxy merger process. We study this dependence in small groups of galaxies. An N-body code is developed which uses an inclination dependent dynamical friction law to affect mergers of galaxies. It is found that some correlation results in this way in groups, which have initially random spin orientations.

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Hoyle, Ben, and Markus Michael Rau. "Self-consistent redshift estimation using correlation functions without a spectroscopic reference sample." Monthly Notices of the Royal Astronomical Society 485, no. 3 (2019): 3642–60. http://dx.doi.org/10.1093/mnras/stz502.

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ABSTRACT We present a new method to estimate redshift distributions and galaxy-dark matter bias parameters using correlation functions in a fully data driven and self-consistent manner. Unlike other machine learning, template, or correlation redshift methods, this approach does not require a reference sample with known redshifts. By measuring the projected cross- and auto-correlations of different galaxy sub-samples, e.g. as chosen by simple cells in colour–magnitude space, we are able to estimate the galaxy-dark matter bias model parameters, and the shape of the redshift distributions of each sub-sample. This method fully marginalizes over a flexible parametrization of the redshift distribution and galaxy-dark matter bias parameters of sub-samples of galaxies, and thus provides a general Bayesian framework to incorporate redshift uncertainty into the cosmological analysis in a data-driven, consistent, and reproducible manner. This result is improved by an order of magnitude by including cross-correlations with the cosmic microwave background and with galaxy–galaxy lensing. We showcase how this method could be applied to real galaxies. By using idealized data vectors, in which all galaxy-dark matter model parameters and redshift distributions are known, this method is demonstrated to recover unbiased estimates on important quantities, such as the offset Δz between the mean of the true and estimated redshift distribution and the 68 per cent, 95 per cent, and 99.5 per cent widths of the redshift distribution to an accuracy required by current and future surveys.

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O’Donnell, Christine, Peter Behroozi, and Surhud More. "Observing correlations between dark matter accretion and galaxy growth: II. testing the impact of galaxy mass, star formation indicator, and neighbour colours." Monthly Notices of the Royal Astronomical Society 509, no. 3 (2021): 3285–300. http://dx.doi.org/10.1093/mnras/stab3170.

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ABSTRACT A crucial question in galaxy formation is what role new accretion has in star formation. Theoretical models have predicted a wide range of correlation strengths between halo accretion and galaxy star formation. Previously, we presented a technique to observationally constrain this correlation strength for isolated Milky Way mass galaxies at z ∼ 0.12, based on the correlation between halo accretion and the density profile of neighbouring galaxies. By applying this technique to both observational data from the Sloan Digital Sky Survey and simulation data from the UniverseMachine, where we can test different correlation strengths, we ruled out positive correlations between dark matter accretion and recent star formation activity. In this work, we expand our analysis by (1) applying our technique separately to red and blue neighbouring galaxies, which trace different infall populations, (2) correlating dark matter accretion rates with Dn 4000 measurements as a longer-term quiescence indicator than instantaneous star-formation rates, and (3) analysing higher-mass isolated central galaxies with 1011.0 &lt; M*/M⊙ &lt; 1011.5 out to z ∼ 0.18. In all cases, our results are consistent with non-positive correlation strengths with ≳ 85 per cent confidence, which is most consistent with models where processes such as gas recycling dominate star formation in massive z = 0 galaxies.

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van Daalen, Marcel P., Bruno M. B. Henriques, Raul E. Angulo, and Simon D. M. White. "The galaxy correlation function as a constraint on galaxy formation physics." Monthly Notices of the Royal Astronomical Society 458, no. 1 (2016): 934–49. http://dx.doi.org/10.1093/mnras/stw405.

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Fry, J. N., and Enrique Gaztanaga. "Redshift distortions of galaxy correlation functions." Astrophysical Journal 425 (April 1994): 1. http://dx.doi.org/10.1086/173956.

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Shen, Zhi, Jun Zhang, Cong Liu, et al. "Tele-correlation: calibrating shear-shear correlation with real data." Journal of Cosmology and Astroparticle Physics 2025, no. 01 (2025): 068. https://doi.org/10.1088/1475-7516/2025/01/068.

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Abstract Tele-correlation refers to the correlation of galaxy shapes with large angular separations (e.g., > 100 degrees). Since there are no astrophysical reasons causing such a correlation on cosmological scales, any detected tele-correlation could disclose systematic effects in shear-shear correlation measurement. If the shear estimators are measured on single exposures, we show that the field distortion (FD) signal associated with the galaxy position on the CCD can be retained and used in tele-correlation to help us directly calibrate the multiplicative and additive biases in shear-shear correlations. We use the DECaLS shear catalog produced by the Fourier_Quad pipeline to demonstrate this idea. To our surprise, we find that significant multiplicative biases can arise (up to more than 10%) due to redshift binning of the galaxies. Correction for this bias leads to about 1σ increase of the best-fit value of S 8 from 0.760+0.015 -0.017 to 0.777+0.016 -0.019 in our tomography study.

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Yamagata, Tomohiko. "Morphological Type Correlation between Nearest Neighbor Pairs of Galaxies." International Astronomical Union Colloquium 124 (1990): 25–31. http://dx.doi.org/10.1017/s0252921100004826.

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Although the morphological type of galaxies is one of the most fundamental properties of galaxies, its origin and evolutionary processes, if any, axe not yet fully understood. It has been established that the galaxy morphology strongly depends on the environment in which the galaxy resides (e.g. Dressler 1980).Galaxy pairs correspond to the smallest scales of galaxy clustering and may provide important clues to how the environment influences the formation and evolution of galaxies. Several investigators pointed out that there is a tendency for pair galaxies to have similar morphological types (Karachentsev and Karachentseva 1974, Page 1975, Noerdlinger 1979).We analyzed morphological type correlation for 18,364 nearest neighbor pairs of galaxies identified in the magnetic tape version of the Center for Astrophysics Redshift Catalogue (Huchra 1987, hereafter CfA Catalog).

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Grimm, Nastassia, Martin Pijnenburg, Giulia Cusin, and Camille Bonvin. "The impact of large-scale galaxy clustering on the variance of the Hellings-Downs correlation: numerical results." Journal of Cosmology and Astroparticle Physics 2025, no. 04 (2025): 047. https://doi.org/10.1088/1475-7516/2025/04/047.

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Abstract Pulsar timing array experiments have recently found evidence for a stochastic gravitational wave (GW) background, which induces correlations among pulsar timing residuals described by the Hellings and Downs (HD) curve. Standard calculations of the HD correlation and its variance assume an isotropic background. However, for a background of astrophysical origin, we expect a higher GW spectral density in directions with higher galaxy number densities. In a companion paper, we have developed a theoretical formalism to account for the anisotropies arising from large-scale galaxy clustering, leading to a new contribution to the variance of the HD correlation. In this subsequent work, we provide numerical results for this novel effect. We consider a GW background resulting from mergers of supermassive black hole binaries, and relate the merger number density to the overdensity of galaxies. We find that anisotropies due to large-scale galaxy clustering lead to a standard deviation of the HD correlation at most at percent level, remaining well below the standard contributions to the HD variance. Hence, this kind of anisotropies in the GW source distribution does not represent a substantial contamination to the correlations of timing residuals in present and future PTA surveys. Suitable statistical methods to extract the galaxy clustering signal from PTA data will be investigated in the future.

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Croft, R. A. C., G. B. Dalton, and G. Efstathiou. "The APM cluster--galaxy cross-correlation function: constraints on and galaxy bias." Monthly Notices of the Royal Astronomical Society 305, no. 3 (1999): 547–62. http://dx.doi.org/10.1046/j.1365-8711.1999.02381.x.

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Gaztanaga, Enrique, and Joshua A. Frieman. "Bias and high-order galaxy correlation functions in the APM galaxy survey." Astrophysical Journal 437 (December 1994): L13. http://dx.doi.org/10.1086/187671.

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Kwan, Juliana, Shun Saito, Alexie Leauthaud, et al. "Galaxy Clustering in the Mira-Titan Universe. I. Emulators for the Redshift Space Galaxy Correlation Function and Galaxy–Galaxy Lensing." Astrophysical Journal 952, no. 1 (2023): 80. http://dx.doi.org/10.3847/1538-4357/acd92f.

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Abstract We construct accurate emulators for the projected and redshift space galaxy correlation functions and excess surface density as measured by galaxy–galaxy lensing, based on halo occupation distribution modeling. Using the complete Mira-Titan suite of 111 N-body simulations, our emulators vary over eight cosmological parameters and include the effects of neutrino mass and dynamical dark energy. We demonstrate that our emulators are sufficiently accurate for the analysis of the Baryon Oscillation Spectroscopic Survey DR12 CMASS galaxy sample over the range 0.5 ≤ r ≤ 50 h −1 Mpc. Furthermore, we show that our emulators are capable of recovering unbiased cosmological constraints from realistic mock catalogs over the same range. Our mock catalog tests show the efficacy of combining small-scale galaxy–galaxy lensing with redshift space clustering and that we can constrain the growth rate and σ 8 to 7% and 4.5%, respectively, for a CMASS-like sample using only the measurements covered by our emulator. With the inclusion of a cosmic microwave background prior on H 0, this reduces to a 2% measurement of the growth rate.

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Collins, C. A. "Galaxy Clustering in the Southern Hemisphere." International Astronomical Union Colloquium 148 (1995): 510–21. http://dx.doi.org/10.1017/s0252921100022454.

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AbstractIn this paper some of the major results from the COSMOS and APM digitised galaxy surveys are presented. The main motivation behind these catalogues was to study large-scale structure in the universe. We begin by outlining the importance of such studies to cosmology and discussing the early results from the visually compiled galaxy catalogues. The impact of the digitised catalogues is demonstrated by focussing on three key areas of research; the galaxy-galaxy two-point angular correlation function, the cluster-cluster spatial correlation function, and galaxy number counts.

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Shanks, T., D. Hale-Sutton, and B. J. Boyle. "Observations of Galaxy and QSO Clustering." Symposium - International Astronomical Union 130 (1988): 371–77. http://dx.doi.org/10.1017/s0074180900136253.

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We present correlation function results from galaxy and QSO redshift surveys. The galaxy correlation function shows evidence for a possible ‘shoulder’ feature in ξ(s) at s = 2h−1 Mpc. At scales between 10 and 100h−1Mpc the correlation function remains close to zero and shows no evidence for any large scale galaxy clustering. The QSO correlation function detects strong QSO clustering for scales s < 10h−1 Mpc. At larger scales (10 < s < 1000h−1 Mpc) no evidence of significant QSO clustering is seen.

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Yuan, Sihan, Boryana Hadzhiyska, Sownak Bose, Daniel J. Eisenstein, and Hong Guo. "Evidence for galaxy assembly bias in BOSS CMASS redshift-space galaxy correlation function." Monthly Notices of the Royal Astronomical Society 502, no. 3 (2021): 3582–98. http://dx.doi.org/10.1093/mnras/stab235.

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ABSTRACT Building accurate and flexible galaxy–halo connection models is crucial in modelling galaxy clustering on non-linear scales. Recent studies have found that halo concentration by itself cannot capture the full galaxy assembly bias effect and that the local environment of the halo can be an excellent indicator of galaxy assembly bias. In this paper, we propose an extended halo occupation distribution (HOD) model that includes both a concentration-based assembly bias term and an environment-based assembly bias term. We use this model to achieve a good fit (χ2/degrees of freedom = 1.35) on the 2D redshift-space two-point correlation function (2PCF) of the Baryon Oscillation Spectroscopic Survey (BOSS) CMASS galaxy sample. We find that the inclusion of both assembly bias terms is strongly favoured by the data and the standard five-parameter HOD model is strongly rejected. More interestingly, the redshift-space 2PCF drives the assembly bias parameters in a way that preferentially assigns galaxies to lower mass haloes. This results in galaxy–galaxy lensing predictions that are within 1σ agreement with the observation, alleviating the perceived tension between galaxy clustering and lensing. We also showcase a consistent 3σ–5σ preference for a positive environment-based assembly bias that persists over variations in the fit. We speculate that the environmental dependence might be driven by underlying processes such as mergers and feedback, but might also be indicative of a larger halo boundaries such as the splashback radius. Regardless, this work highlights the importance of building flexible galaxy–halo connection models and demonstrates the extra constraining power of the redshift-space 2PCF.

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Lee, S., M. A. Troxel, A. Choi, et al. "Galaxy–galaxy lensing with the DES-CMASS catalogue: measurement and constraints on the galaxy-matter cross-correlation." Monthly Notices of the Royal Astronomical Society 509, no. 2 (2021): 2033–47. http://dx.doi.org/10.1093/mnras/stab3028.

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ABSTRACT The DMASS sample is a photometric sample from the DES Year 1 data set designed to replicate the properties of the CMASS sample from BOSS, in support of a joint analysis of DES and BOSS beyond the small overlapping area. In this paper, we present the measurement of galaxy–galaxy lensing using the DMASS sample as gravitational lenses in the DES Y1 imaging data. We test a number of potential systematics that can bias the galaxy–galaxy lensing signal, including those from shear estimation, photometric redshifts, and observing conditions. After careful systematic tests, we obtain a highly significant detection of the galaxy–galaxy lensing signal, with total S/N = 25.7. With the measured signal, we assess the feasibility of using DMASS as gravitational lenses equivalent to CMASS, by estimating the galaxy-matter cross-correlation coefficient rcc. By jointly fitting the galaxy–galaxy lensing measurement with the galaxy clustering measurement from CMASS, we obtain $r_{\rm cc}=1.09^{+0.12}_{-0.11}$ for the scale cut of $4 \, h^{-1}{\rm \,\,Mpc}$ and $r_{\rm cc}=1.06^{+0.13}_{-0.12}$ for $12 \, h^{-1}{\rm \,\,Mpc}$ in fixed cosmology. By adding the angular galaxy clustering of DMASS, we obtain rcc = 1.06 ± 0.10 for the scale cut of $4 \, h^{-1}{\rm \,\,Mpc}$ and rcc = 1.03 ± 0.11 for $12 \, h^{-1}{\rm \,\,Mpc}$. The resulting values of rcc indicate that the lensing signal of DMASS is statistically consistent with the one that would have been measured if CMASS had populated the DES region within the given statistical uncertainty. The measurement of galaxy–galaxy lensing presented in this paper will serve as part of the data vector for the forthcoming cosmology analysis in preparation.

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Chown, Ryan, Cheng Li, Laura Parker, Christine D. Wilson, Niu Li, and Yang Gao. "A new estimator of resolved molecular gas in nearby galaxies." Monthly Notices of the Royal Astronomical Society 500, no. 1 (2020): 1261–78. http://dx.doi.org/10.1093/mnras/staa3288.

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ABSTRACT A relationship between dust-reprocessed light from recent star formation and the amount of star-forming gas in a galaxy produces a correlation between Wide-field Infrared Survey Explorer (WISE) 12 μm emission and CO line emission. Here, we explore this correlation on kiloparsec scales with CO(1–0) maps from EDGE–CALIFA matched in resolution to WISE 12 μm images. We find strong CO-12 μm correlations within each galaxy and we show that the scatter in the global CO-12 μm correlation is largely driven by differences from galaxy to galaxy. The correlation is stronger than that between star formation rate and H2 surface densities [Σ(H2)]. We explore multivariable regression to predict Σ(H2) in star-forming pixels using the WISE 12 μm data combined with global and resolved galaxy properties, and provide the fit parameters for the best estimators. We find that Σ(H2) estimators that include $\Sigma (\mathrm{12\:\mu m})$ are able to predict Σ(H2) more accurately than estimators that include resolved optical properties instead of $\Sigma (\mathrm{12\:\mu m})$. These results suggest that 12 μm emission and H2 as traced by CO emission are physically connected at kiloparsec scales. This may be due to a connection between polycyclic aromatic hydrocarbon emission and the presence of H2. The best single-property estimator is $\log \frac{\Sigma (\mathrm{H_2})}{\mathrm{M_\odot \:pc^{-2}}} = (0.48 \pm 0.01) + (0.71 \pm 0.01)\log \frac{\Sigma (\mathrm{12\:\mu m})}{\mathrm{L_\odot \:pc^{-2}}}$. This correlation can be used to efficiently estimate Σ(H2) down to at least 1 M⊙ pc−2 in star-forming regions within nearby galaxies.

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Kable, Joshua A., Giampaolo Benevento, Noemi Frusciante, Antonio De Felice, and Shinji Tsujikawa. "Probing modified gravity with integrated Sachs-Wolfe CMB and galaxy cross-correlations." Journal of Cosmology and Astroparticle Physics 2022, no. 09 (2022): 002. http://dx.doi.org/10.1088/1475-7516/2022/09/002.

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Abstract We use the cross-correlation power spectrum of the integrated Sachs-Wolfe (ISW) effect in the cosmic microwave background (CMB) temperature anisotropy and galaxy fluctuations to probe the physics of late-time cosmic acceleration. For this purpose, we focus on three models of dark energy that belong to a sub-class of Horndeski theories with the speed of gravity equivalent to that of light: Galileon Ghost Condensate (GGC), Generalized Cubic Covariant Galileon (GCCG), and K-mouflage. In the GGC and GCCG models, the existence of cubic-order scalar self-interactions allows a possibility for realizing negative ISW-galaxy cross-correlations, while the K-mouflage model predicts a positive correlation similar to the Λ-cold-dark-matter (ΛCDM) model. In our analysis, we fix the parameters of each model to their best-fit values derived from a baseline likelihood analysis with observational data from CMB, baryon acoustic oscillations, and supernovae type Ia. Then we fit those best-fit models to the ISW-galaxy cross-correlation power spectrum extracted from a collection of photometric redshift surveys. We find that both GGC and GCCG best-fit models degrade the fit to the ISW-galaxy cross-correlation data compared to ΛCDM best-fit model. This is attributed to the fact that, for their best-fit values constrained from the baseline likelihood, the cubic-order scalar self-interaction gives rise to suppressed ISW tails relative to ΛCDM. The K-mouflage best-fit model is largely degenerate with the ΛCDM best-fit model and has a positively correlated ISW-galaxy power close to that of ΛCDM.

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Stevenson, P. R. F., T. Shanks, R. Fong, and H. T. MacGillivray. "Correlation analyses of deep galaxy samples - III." Monthly Notices of the Royal Astronomical Society 213, no. 4 (1985): 953–69. http://dx.doi.org/10.1093/mnras/213.4.953.

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Lee, Jounghun, and Ue‐Li Pen. "Galaxy Spin Statistics and Spin‐Density Correlation." Astrophysical Journal 555, no. 1 (2001): 106–24. http://dx.doi.org/10.1086/321472.

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Marin, Felipe A., Risa H. Wechsler, Joshua A. Frieman, and Robert C. Nichol. "Modeling the Galaxy Three‐Point Correlation Function." Astrophysical Journal 672, no. 2 (2008): 849–60. http://dx.doi.org/10.1086/523628.

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Pons‐Borderia, Maria‐Jesus, Vicent J. Martinez, Dietrich Stoyan, Helga Stoyan, and Enn Saar. "Comparing Estimators of the Galaxy Correlation Function." Astrophysical Journal 523, no. 2 (1999): 480–91. http://dx.doi.org/10.1086/307754.

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Benevento, G., N. Bartolo, and M. Liguori. "ISW-galaxy cross-correlation in K-mouflage." Journal of Physics: Conference Series 956 (January 2018): 012001. http://dx.doi.org/10.1088/1742-6596/956/1/012001.

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Iqbal, Naseer, Naveel Ahmad, Mubashir Hamid, and Tabasum Masood. "Correlation functions for extended mass galaxy clusters." Monthly Notices of the Royal Astronomical Society: Letters 424, no. 1 (2012): L31—L33. http://dx.doi.org/10.1111/j.1745-3933.2012.01281.x.

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40

Salvador-Sole, Eduard, and Manuel Sanroma. "Study of galaxy structures by correlation analysis." Astrophysical Journal 345 (October 1989): 660. http://dx.doi.org/10.1086/167939.

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Wakeel Khanday, Abdul. "A Simplistic Approach to the Study of Two-Point Correlation Function in Galaxy Clusters." Open Access Journal of Astronomy 2, no. 2 (2024): 1–7. http://dx.doi.org/10.23880/oaja-16000127.

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We developed the functional form of the two-point correlation function under the approximation of fixed particle number density. We solved the quasi-linear partial differential equation (PDE) through the method of characteristics to obtain the parametric solution for the canonical ensemble. We attempted many functional forms and concluded that the functional form should be such that the two-point correlation function should go to zero as the value of system temperature increases or the separation between the galaxies becomes large. Also we studied the graphical behavior of the developed two-point correlation function for large values of temperature T and spatial separation r. The behavior of the two-point function was also studied from the temperature measurement of clusters in the red-shift range of 0.023-0.546.

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Sullivan, James M., Uroš Seljak, and Sukhdeep Singh. "An analytic hybrid halo + perturbation theory model for small-scale correlators: baryons, halos, and galaxies." Journal of Cosmology and Astroparticle Physics 2021, no. 11 (2021): 026. http://dx.doi.org/10.1088/1475-7516/2021/11/026.

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Abstract We update Halo Zeldovich Perturbation Theory (HZPT, [1]), an analytic model for the two-point statistics of dark matter, to describe halo and galaxy clustering, and galaxy-matter cross-correlation on nonlinear scales. The model correcting Zeldovich has an analytic Fourier transform, and therefore is valid in both configuration space and Fourier space. The model is accurate at the 2%-level or less for P_mm (k< 1 h/Mpc), P_hm (k< 1 h/Mpc), P_hh (k< 2 h/Mpc), Pgm (k< 1 h/Mpc), Pgg (k< 1 h/Mpc), ξmm (r> 1 Mpc/h), ξhm (r> 2 Mpc/h), ξhh (r> 2 Mpc/h), ξgm (r> 1 Mpc/h), ξgg (r> 2 Mpc/h), for LRG-like mock galaxies. We show that the HZPT model for matter correlators can account for the effects of a wide range of baryonic feedback models and provide two extended dark matter models which are of 1% (3%) accuracy for k < 10 (8) h/Mpc. We explicitly model the non-perturbative features of halo exclusion for the halo-halo and galaxy-galaxy correlators, as well as the presence of satellites for galaxy-matter and galaxy-galaxy correlation functions. We perform density estimation using N-body simulations and a wide range of HOD galaxy mocks to obtain correlations of model parameters with the cosmological parameters Ωm and σ8. HZPT can provide a fast, interpretable, and analytic model for combined-probe analyses of redshift surveys using scales well into the non-linear regime.

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Tian, H. J., M. C. Neyrinck, T. Budavári, and A. S. Szalay. "The Enhancement of BAO in the SDSS MGS." Proceedings of the International Astronomical Union 11, S319 (2015): 145. http://dx.doi.org/10.1017/s1743921315010042.

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AbstractWe show that redshift-space distortions of galaxy correlations have a strong effect on correlation functions with the signature of the Baryon Acoustic Oscillations (BAO). Near the line of sight, the features become sharper as a result of redshift-space distortions. We analyze the SDSS DR7 main-galaxy sample (MGS), splitting the sample into slices 2.5 deg on the sky in various rotations. Measuring 2D correlation functions in each slice, we do see a sharp bump along the line of sight. Using Mexican-hat wavelets, we localize it to (110 ± 10) h − 1 Mpc and estimate its significance at about 4σ.

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Makiya, Ryu, and Tomomi Sunayama. "Mitigating the impact of fiber assignment on the measurement of galaxy-lensing cross correlation." Journal of Cosmology and Astroparticle Physics 2022, no. 03 (2022): 008. http://dx.doi.org/10.1088/1475-7516/2022/03/008.

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Abstract We examine the impact of fiber assignment on the measurement of galaxy clustering and its cross correlation with weak lensing fields. Unlike the past spectroscopic galaxy surveys such as Baryon Oscillation Spectroscopic Survey (BOSS), currently ongoing spectroscopic galaxy surveys such as Prime Focus Spectrograph (PFS) and Dark Energy Spectroscopic Instrument (DESI) suffer from the fiber assignment artifacts more severely because there are more target galaxies than available fibers. The previous studies found that the fiber assignment suppresses the amplitude of the galaxy power spectrum at all scales. We newly find that the fiber assignment introduces the artificial correlation of structure at different redshifts, which suppresses the amplitude of the galaxy-lensing cross power spectrum. We show that the fiber assignment effects on the cross power spectrum can be mitigated at all scales with accuracy better than ∼ 1%, by up-weighting observed galaxies with the probability to be observed. This is not the case for the galaxy power spectrum, which is not fully corrected at k ≳ 0.2 [h/Mpc]. We find that the galaxy-lensing cross power spectrum is not affected by the pairwise probability of galaxies to be observed, and thus the correction method based on the individual probability is sufficient at all scales.

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45

Rafiei-Ravandi, Masoud, Kendrick M. Smith, D. Michilli, et al. "Statistical Association between the Candidate Repeating FRB 20200320A and a Galaxy Group." Astrophysical Journal 961, no. 2 (2024): 177. http://dx.doi.org/10.3847/1538-4357/ad0c59.

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Abstract We present results from angular cross correlations between select samples of CHIME/FRB repeaters and galaxies in three photometric galaxy surveys, which have shown correlations with the first CHIME/FRB catalog containing repeating and nonrepeating sources: Wide-field Infrared Survey Explorer (WISE) × SCOS, DESI-BGS, and DESI-LRG. We find a statistically significant correlation (p-value <0.001, after accounting for look-elsewhere factors) between a sample of repeaters with an extragalactic dispersion measure (DM) > 395 pc cm−3 and WISE × SCOS galaxies with redshift z > 0.275. We demonstrate that the correlation arises surprisingly because of a statistical association between FRB 20200320A (extragalactic DM ≈ 550 pc cm−3) and a galaxy group in the same dark matter halo at redshift z ≈ 0.32. We estimate that the host halo, along with an intervening halo at redshift z ≈ 0.12, accounts for at least ∼30% of the extragalactic DM. Our results strongly motivate incorporating galaxy group and cluster catalogs into direct host association pipelines for FRBs with ≲ 1 ′ localization precision, effectively utilizing the two-point information to constrain FRB properties such as their redshift and DM distributions. In addition, we find marginal evidence for a negative correlation at 99.4% confidence limit between a sample of repeating FRBs with baseband data (median extragalactic DM = 354 pc cm−3) and DESI-LRG galaxies with redshift 0.3 ≤ z < 0.45, suggesting that the repeaters might be more prone than apparent nonrepeaters to propagation effects in FRB–galaxy correlations due to intervening free electrons over angular scales ∼0.°5.

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46

Adelberger, Kurt L. "Estimating the Galaxy Correlation Lengthr0from the Number of Galaxy Pairs with Similar Redshifts." Astrophysical Journal 621, no. 2 (2005): 574–81. http://dx.doi.org/10.1086/427917.

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47

Lidman, C. E., and B. A. peterson. "Galaxy counts and the galaxy two-point angular correlation function to I=23." Monthly Notices of the Royal Astronomical Society 279, no. 4 (1996): 1357–79. http://dx.doi.org/10.1093/mnras/279.4.1357.

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48

Goldman, T., D. Hochberg, R. Laflamme, and J. Pérez-Mercader. "The galaxy-galaxy correlation function as an indicator of critical phenomena in cosmology." Physics Letters A 222, no. 3 (1996): 177–81. http://dx.doi.org/10.1016/0375-9601(96)00588-9.

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49

Chisari, Nora Elisa, Joanna Dunkley, Lance Miller, and Rupert Allison. "Contamination of early-type galaxy alignments to galaxy lensing–CMB lensing cross-correlation." Monthly Notices of the Royal Astronomical Society 453, no. 1 (2015): 682–89. http://dx.doi.org/10.1093/mnras/stv1655.

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Johnston, D. E. "Measuring the galaxy-galaxy-mass three-point correlation function with weak gravitational lensing." Monthly Notices of the Royal Astronomical Society 367, no. 3 (2006): 1222–40. http://dx.doi.org/10.1111/j.1365-2966.2006.10011.x.

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