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Journal articles on the topic 'Galaxy'

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Author: Grafiati

Published: 4 June 2021

Last updated: 6 September 2023

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1

Wilson, Gillian, Nick Kaiser, Gerard A. Luppino, and Lennox L. Cowie. "Galaxy Halo Masses from Galaxy‐Galaxy Lensing." Astrophysical Journal 555, no. 2 (July 10, 2001): 572–84. http://dx.doi.org/10.1086/321441.

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2

Saghiha, H., S. Hilbert, P. Schneider, and P. Simon. "Galaxy-galaxy(-galaxy) lensing as a sensitive probe of galaxy evolution." Astronomy & Astrophysics 547 (October 31, 2012): A77. http://dx.doi.org/10.1051/0004-6361/201219358.

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3

Mao, Shude, Jian Wang, and Martin C. Smith. "Moderate galaxy-galaxy lensing." Monthly Notices of the Royal Astronomical Society 422, no. 4 (April 24, 2012): 2808–15. http://dx.doi.org/10.1111/j.1365-2966.2012.20438.x.

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4

Anthony Tyson, J. "Galaxy Mass Distribution from Galaxy-Galaxy Gravitational Lensing." Symposium - International Astronomical Union 117 (1987): 241. http://dx.doi.org/10.1017/s0074180900150259.

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The average gravitational lens distortion of background galaxy images by foreground galaxies is an independent, non-kinematical measurement of galaxy mass distribution M(r)/r (Tyson, et al. 1984). The upper limit we obtained for the equivalent circular velocity, while small compared with some heavy halo models, is consistent with dynamical estimates for samples of galaxies of all types (e.g. Turner's binary data and the Rubin, et al. rotation curves). For example, for a mean cutoff radius of 65 kpc/h, our 3σ upper limit for the equivalent circular velocity (GM/r)1/2 = 190 km/sec. For a mass cutoff at 190 kpc/h our 2σ upper limit is 175 km/sec. If I weight a sample of asymptotical rotation curve velocities by recent field luminosity functions, I get mean circular velocities less than 170 km/sec.

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Simon, P., T. Erben, P. Schneider, C. Heymans, H. Hildebrandt, H. Hoekstra, T. D. Kitching, et al. "CFHTLenS: higher order galaxy–mass correlations probed by galaxy–galaxy–galaxy lensing." Monthly Notices of the Royal Astronomical Society 430, no. 3 (February 7, 2013): 2476–98. http://dx.doi.org/10.1093/mnras/stt069.

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Simon, P., P. Watts, P. Schneider, H. Hoekstra, M. D. Gladders, H. K. C. Yee, B. C. Hsieh, and H. Lin. "First detection of galaxy-galaxy-galaxy lensing in RCS." Astronomy & Astrophysics 479, no. 3 (January 2, 2008): 655–67. http://dx.doi.org/10.1051/0004-6361:20078197.

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Cohn, J. D. "Galaxy subgroups in galaxy clusters." Monthly Notices of the Royal Astronomical Society 419, no. 2 (October 21, 2011): 1017–27. http://dx.doi.org/10.1111/j.1365-2966.2011.19756.x.

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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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Renneby, Malin, Bruno M. B. Henriques, Stefan Hilbert, Dylan Nelson, Mark Vogelsberger, Raúl E. Angulo, Volker Springel, and Lars Hernquist. "Joint galaxy–galaxy lensing and clustering constraints on galaxy formation." Monthly Notices of the Royal Astronomical Society 498, no. 4 (September 4, 2020): 5804–33. http://dx.doi.org/10.1093/mnras/staa2675.

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ABSTRACT We compare predictions for galaxy–galaxy lensing profiles and clustering from the Henriques et al. public version of the Munich semi-analytical model (SAM) of galaxy formation and the IllustrisTNG suite, primarily TNG300, with observations from KiDS + GAMA and SDSS-DR7 using four different selection functions for the lenses (stellar mass, stellar mass and group membership, stellar mass and isolation criteria, and stellar mass and colour). We find that this version of the SAM does not agree well with the current data for stellar mass-only lenses with $M_\ast \gt 10^{11}\, \mathrm{ M}_\odot$. By decreasing the merger time for satellite galaxies as well as reducing the radio-mode active galactic nucleus accretion efficiency in the SAM, we obtain better agreement, both for the lensing and the clustering, at the high-mass end. We show that the new model is consistent with the signals for central galaxies presented in Velliscig et al. Turning to the hydrodynamical simulation, TNG300 produces good lensing predictions, both for stellar mass-only (χ2 = 1.81 compared to χ2 = 7.79 for the SAM) and locally brightest galaxy samples (χ2 = 3.80 compared to χ2 = 5.01). With added dust corrections to the colours it matches the SDSS clustering signal well for red low-mass galaxies. We find that both the SAMs and TNG300 predict $\sim 50\, {{\ \rm per\ cent}}$ excessive lensing signals for intermediate-mass red galaxies with 10.2 < log10M*[M⊙] < 11.2 at $r \approx 0.6\, h^{-1}\, \text{Mpc}$, which require further theoretical development.

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10

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

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11

Linke, Laila, Patrick Simon, Peter Schneider, Thomas Erben, Daniel J. Farrow, Catherine Heymans, Hendrik Hildebrandt, et al. "KiDS+VIKING+GAMA: Testing semi-analytic models of galaxy evolution with galaxy–galaxy–galaxy lensing." Astronomy & Astrophysics 640 (August 2020): A59. http://dx.doi.org/10.1051/0004-6361/202038355.

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Context. Several semi-analytic models (SAMs) try to explain how galaxies form, evolve, and interact inside the dark matter large-scale structure. These SAMs can be tested by comparing their predictions for galaxy–galaxy–galaxy lensing (G3L), which is weak gravitational lensing around galaxy pairs, with observations. Aims. We evaluate the SAMs by Henriques et al. (2015, MNRAS, 451, 2663, hereafter H15) and by Lagos et al. (2012, MNRAS, 426, 2142, hereafter L12), which were implemented in the Millennium Run, by comparing their predictions for G3L to observations at smaller scales than previous studies and also for pairs of lens galaxies from different populations. Methods. We compared the G3L signal predicted by the SAMs to measurements in the overlap of the Galaxy And Mass Assembly survey (GAMA), the Kilo-Degree Survey (KiDS), and the VISTA Kilo-degree Infrared Galaxy survey (VIKING) by splitting lens galaxies into two colour and five stellar-mass samples. Using an improved G3L estimator, we measured the three-point correlation of the matter distribution with “mixed lens pairs” with galaxies from different samples, and with “unmixed lens pairs” with galaxies from the same sample. Results. Predictions by the H15 SAM for the G3L signal agree with the observations for all colour-selected samples and all but one stellar-mass-selected sample with 95% confidence. Deviations occur for lenses with stellar masses below 9.5 h−2 M⊙ at scales below 0.2 h−1 Mpc. Predictions by the L12 SAM for stellar-mass selected samples and red galaxies are significantly higher than observed, while the predicted signal for blue galaxy pairs is too low. Conclusions. The L12 SAM predicts more pairs of low stellar mass and red galaxies than the H15 SAM and the observations, as well as fewer pairs of blue galaxies. This difference increases towards the centre of the galaxies’ host halos. Likely explanations are different treatments of environmental effects by the SAMs and different models of the initial mass function. We conclude that G3L provides a stringent test for models of galaxy formation and evolution.

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Bois, Yve-Alain. "Galaxy." October 108 (April 2004): 28–34. http://dx.doi.org/10.1162/octo.2004.108.1.28.

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13

Moscoso-Sánchez, David-Jesús. "From Gutenberg galaxy to Internet galaxy." Comunicar 12, no. 23 (October 1, 2004): 124–28. http://dx.doi.org/10.3916/c23-2004-21.

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Reading, like writing is the most important human communication tool excluding spoken language. As language, writing and therefore reading changes through times with regards to elements that go beyond the act of reading. In our days reading in a book or via any digital technology, shows a new model that we characterize here mainly by its flexibility. This paper undertakes the way of reading is actively built through social changes becoming a window to understand society. La lectura, como la escritura, es el instrumento por antonomasia de la comunicación humana, si exceptuamos al lenguaje hablado. Como el lenguaje, la escritura y, por tanto, la lectura, cambian de forma en el tiempo, en razón de elementos que trascienden el mero acto de leer. En nuestra época, la lectura, ya sea a través del papel o de cualquier tecnología digital, evidencia un nuevo canon que aquí caracterizamos principalmente por su flexibilidad. Este artículo aborda el modo en que la lectura se construye activamente a través de los procesos de cambio social, convirtiéndose en sí misma en una ventana a través de la cual conocer cómo es una sociedad.

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14

Schneider, Peter, and Hans‐Walter Rix. "Quantitative Analysis of Galaxy‐Galaxy Lensing." Astrophysical Journal 474, no. 1 (January 1997): 25–36. http://dx.doi.org/10.1086/303435.

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15

Driver, Simon P., Jochen Liske, and Alister W. Graham. "The Millennium Galaxy Catalogue: Galaxy Bimodality." Proceedings of the International Astronomical Union 2, S235 (August 2006): 17–18. http://dx.doi.org/10.1017/s1743921306004960.

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AbstractGalaxy bimodality is caused by the bulge-disc nature of galaxies as opposed to two distinct galaxy classes. This is evident in the colour-structure plane which clearly shows that elliptical galaxies (bulge-only) lie in the red compact peak and late-type spiral galaxies (disc-dominated) lie in the blue diffuse peak. Early-type spirals (bulge plus disc systems) sprawl across both peaks. However after bulge-disc decomposition the bulges of early-type spirals lie exclusively in the red compact peak and their discs in the blue diffuse peak (exceptions exist but are rare, e.g., dust reddened edge-on discs and blue pseudo-bulges). Movement between these two peaks is not trivial because whilst switching off star-formation can transform colours from blue to red, modifying the orbits of ~1 billion stars from a planar diffuse structure to a triaxial compact structure is problematic (essentially requiring an equal mass merger). We propose that the most plausible explanation for the dual structure of galaxies is that galaxy formation proceeds in two stages. First an initial collapse phase (forming a centrally concentrated core and black hole), followed by splashback, infall and accretion (forming a planar rotating disc). Dwarf systems coule perhaps follow the same scenario but the lack of low luminosity bulge-disc systems would imply that the two components must rapidly blend to form a single flattened spheroidal system.

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16

Gardner, J. P. "Galaxy Evolution from Deep Galaxy Counts." Symposium - International Astronomical Union 164 (1995): 311–19. http://dx.doi.org/10.1017/s007418090010871x.

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We present deep galaxy number counts and colours of K – band selected galaxy surveys. We argue that primeval galaxies are present within the survey data, but have remained unidentified. There are few objects with the colours of an L∗ elliptical galaxy at a redshift of z ≈ 1, in contradiction to standard luminosity evolution models. We present K – band photometry of the objects in a spectroscopic redshift survey selected at 21 < B < 22.5. The absolute K magnitudes of the galaxies are consistent with the no-evolution or pure luminosity evolution models. The excess faint blue galaxies seen in the B – band number counts at intermediate magnitudes are a result of a low normalization, and do not dominate the population until B ≈ 25. Extreme merging or excess dwarf models are not needed at z < 1.

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17

Brainerd, Tereasa G. "Galaxy-Galaxy Lensing: Status & Applications." Symposium - International Astronomical Union 201 (2005): 282–91. http://dx.doi.org/10.1017/s0074180900216367.

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There are now 10 independent observational investigations which have detected systematic weak gravitational lensing of background field galaxies by foreground field galaxies. This effect, known as galaxy-galaxy lensing, results in a very slight (of order 1%) distortion to the intrinsic image shapes of the lensed galaxies. Although small, the galaxy-galaxy lensing signal is coherent about the lens centers and is, therefore, detectable in large data sets via an ensemble average over many candidate pairs of lenses and sources. Here I summarize the results of the recent detections of galaxy-galaxy lensing and discuss some applications that are likely to be implemented in the very near future.

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18

Dell'Antonio, Ian P., and J. Anthony Tyson. "Galaxy Dark Matter: Galaxy-Galaxy Lensing in the Hubble Deep Field." Astrophysical Journal 473, no. 1 (December 10, 1996): L17—L20. http://dx.doi.org/10.1086/310378.

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19

Hikage, Chiaki, Rachel Mandelbaum, Alexie Leauthaud, Eduardo Rozo, and Eli S. Rykoff. "Testing redMaPPer centring probabilities using galaxy clustering and galaxy–galaxy lensing." Monthly Notices of the Royal Astronomical Society 480, no. 2 (July 27, 2018): 2689–97. http://dx.doi.org/10.1093/mnras/sty2013.

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20

Schneider, P., and P. Watts. "Galaxy-galaxy-galaxy lensing: Third-order correlations between the galaxy and mass distributions in the Universe." Astronomy & Astrophysics 432, no. 3 (March 2005): 783–95. http://dx.doi.org/10.1051/0004-6361:20041923.

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21

Lobachev, Yuriy Viktorovich, and Valeriy Tikonovich Krasilnikov. "The effect of new tank mixtures and herbicide compositions on economically useful indicators of soy." Agrarian Scientific Journal, no. 2 (February 19, 2020): 16–23. http://dx.doi.org/10.28983/asj.y2020i2pp16-23.

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The method of two-way analysis of variance in three field experiments in the conditions of the Right Bank of the Saratov Region studied the effect of four herbicides, two new tank mixtures and two new herbicide compositions on grain yield, number of plants per square meter, number of beans per plant, number of grains per plant, plant mass, the mass of beans from the plant, the mass of grain from the plant, the mass of 1000 grains, the protein content in the grain, the height of the plant, the height of attachment of the lower bean. The effectiveness of the herbicides was as follows: frontier optima - 72.5%, pulsar - 26.5%, gezagard - 71.2%, galaxy top - 11.7%, tank mixture frontier optima + gezagard - 86.4%, tank mixture pulsar + galaxy top - 23.0%, composition frontier optima + galaxy top - 73.8%, and composition gezagard + galaxy top - 85.1%. It was established a significant advantage in grain yield of only one new tank mixture of herbicides frontier optima + gezagard and two new compositions of herbicides frontier optima + galaxy top and gezagard + galaxy top. In the case of application of a tank mixture of herbicides, the frontier optima + hezagard yields of soybean grain significantly increased compared with the control by 377.0%, compared with herbicides the frontier optima and hezagard - by 154.0%. After the application of the herbicidal composition, the frontier optima + galaxi top soybean grain yield significantly increased compared with the control by 293.3%, compared with the herbicide frontier optima - by 120.1%, compared with the herbicide galaxy top - by 139.3%. After application of the hezagard + galaxy top herbicide composition, the soybean grain yield significantly increased compared with the control by 294.3%, compared with the hezagard herbicide - by 121.7%, compared with the galaxy top herbicide - by 141.1%.

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Guzik, J., and U. Seljak. "Galaxy--dark matter correlations applied to galaxy--galaxy lensing: predictions from the semi-analytic galaxy formation models." Monthly Notices of the Royal Astronomical Society 321, no. 3 (March 1, 2001): 439–49. http://dx.doi.org/10.1046/j.1365-8711.2001.04081.x.

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Holwerda, B. W., I. K. Baldry, M. Alpaslan, A. Bauer, J. Bland-Hawthorn, S. Brough, M. J. I. Brown, et al. "Galaxy And Mass Assembly (GAMA) blended spectra catalogue: strong galaxy–galaxy lens and occulting galaxy pair candidates." Monthly Notices of the Royal Astronomical Society 449, no. 4 (April 2015): 4277–87. http://dx.doi.org/10.1093/mnras/stv589.

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24

Rasheed, Mariwan A. "SIMULATION OF INTERACTING GALAXY PAIR ARP 82." International Journal of Scientific Research 2, no. 8 (June 1, 2012): 68–70. http://dx.doi.org/10.15373/22778179/aug2013/151.

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25

Rasheed, Mariwan A. "Simulation of Whirlpool Galaxy and its Companion." Journal of Zankoy Sulaimani - Part A 12, no. 1 (July 2, 2008): 125–35. http://dx.doi.org/10.17656/jzs.10203.

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26

Robertson, Andrew. "The galaxy–galaxy strong lensing cross-sections of simulated ΛCDM galaxy clusters." Monthly Notices of the Royal Astronomical Society: Letters 504, no. 1 (March 22, 2021): L7—L11. http://dx.doi.org/10.1093/mnrasl/slab028.

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ABSTRACT We investigate a recent claim that observed galaxy clusters produce an order of magnitude more galaxy–galaxy strong lensing (GGSL) than simulated clusters in a Λ cold dark matter (CDM) cosmology. We take galaxy clusters from the c-eagle hydrodynamical simulations and calculate the expected amount of GGSL for sources placed behind the clusters at different redshifts. The probability of a source lensed by one of the most massive c-eagle clusters being multiply imaged by an individual cluster member is in good agreement with that inferred for observed clusters. We show that numerically converged results for the GGSL probability require higher resolution simulations than had been used previously. On top of this, different galaxy formation models predict cluster substructures with different central densities, such that the GGSL probabilities in ΛCDM cannot yet be robustly predicted. Overall, we find that GGSL within clusters is not currently in tension with the ΛCDM cosmological model.

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Demetroullas, C., and M. L. Brown. "Galaxy–galaxy and galaxy–cluster lensing with the SDSS and FIRST surveys." Monthly Notices of the Royal Astronomical Society 473, no. 1 (September 15, 2017): 937–52. http://dx.doi.org/10.1093/mnras/stx2366.

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Prat, J., C. Sánchez, R. Miquel, J. Kwan, J. Blazek, C. Bonnett, A. Amara, et al. "Galaxy bias from galaxy–galaxy lensing in the DES science verification data." Monthly Notices of the Royal Astronomical Society 473, no. 2 (September 25, 2017): 1667–84. http://dx.doi.org/10.1093/mnras/stx2430.

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Böhm, Vanessa, Chirag Modi, and Emanuele Castorina. "Lensing corrections on galaxy-lensing cross correlations and galaxy-galaxy auto correlations." Journal of Cosmology and Astroparticle Physics 2020, no. 03 (March 20, 2020): 045. http://dx.doi.org/10.1088/1475-7516/2020/03/045.

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Jain, Bhuvnesh, Ryan Scranton, and Ravi K. Sheth. "Quasar-galaxy and galaxy-galaxy cross-correlations: model predictions with realistic galaxies." Monthly Notices of the Royal Astronomical Society 345, no. 1 (October 2003): 62–70. http://dx.doi.org/10.1046/j.1365-8711.2003.06965.x.

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31

Yoo, Jaiyul, Jeremy L. Tinker, David H. Weinberg, Zheng Zheng, Neal Katz, and Romeel Dave. "From Galaxy‐Galaxy Lensing to Cosmological Parameters." Astrophysical Journal 652, no. 1 (November 20, 2006): 26–42. http://dx.doi.org/10.1086/507591.

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32

Pfister, Hugo, Massimo Dotti, Clotilde Laigle, Yohan Dubois, and Marta Volonteri. "Real galaxy mergers from galaxy pair catalogues." Monthly Notices of the Royal Astronomical Society 493, no. 1 (January 29, 2020): 922–29. http://dx.doi.org/10.1093/mnras/staa227.

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ABSTRACT Mergers of galaxies are extremely violent events shaping their evolution. Such events are thought to trigger starbursts and, possibly, black hole accretion. Nonetheless, it is still not clear how to know the fate of a galaxy pair from the data available at a given time, limiting our ability to constrain the exact role of mergers. In this paper we use the light-cone of the horizon-agn simulation, for which we know the fate of each pair, to test three selection processes aiming at identifying true merging pairs. We find that the simplest one (selecting objects within two thresholds on projected distance d and redshift difference Δz) gives similar results than the most complex one (based on a neural network analysing d, Δz, redshift of the primary, masses/star formation rates/aspect ratio of both galaxies). Our best thresholds are $d_\mathrm{th}\sim 100\, \mathrm{kpc}$ and Δzth ∼ 10−3, in agreement with recent results.

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Benavides, José A., Laura V. Sales, and Mario G. Abadi. "Accretion of galaxy groups into galaxy clusters." Monthly Notices of the Royal Astronomical Society 498, no. 3 (September 2, 2020): 3852–62. http://dx.doi.org/10.1093/mnras/staa2636.

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ABSTRACT We study the role of group infall in the assembly and dynamics of galaxy clusters in ΛCDM. We select 10 clusters with virial mass M200 ∼ 1014 $\rm M_\odot$ from the cosmological hydrodynamical simulation Illustris and follow their galaxies with stellar mass M⋆ ≥ 1.5 × 108 $\rm M_\odot$. A median of ${\sim}38{{\ \rm per\ cent}}$ of surviving galaxies at z = 0 is accreted as part of groups and did not infall directly from the field, albeit with significant cluster-to-cluster scatter. The evolution of these galaxy associations is quick, with observational signatures of their common origin eroding rapidly in 1–3 Gyr after infall. Substructure plays a dominant role in fostering the conditions for galaxy mergers to happen, even within the cluster environment. Integrated over time, we identify (per cluster) an average of 17 ± 9 mergers that occur in infalling galaxy associations, of which 7 ± 3 occur well within the virial radius of their cluster hosts. The number of mergers shows large dispersion from cluster to cluster, with our most massive system having 42 mergers above our mass cut-off. These mergers, which are typically gas rich for dwarfs and a combination of gas rich and gas poor for M⋆ ∼ 1011 $\rm M_\odot$, may contribute significantly within ΛCDM to the formation of specific morphologies, such as lenticulars (S0) and blue compact dwarfs in groups and clusters.

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Hwang, Ho Seong, and Myung Gyoon Lee. "Galaxy activity in merging binary galaxy clusters." Monthly Notices of the Royal Astronomical Society 397, no. 4 (August 21, 2009): 2111–22. http://dx.doi.org/10.1111/j.1365-2966.2009.15100.x.

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Kleinheinrich, Martina, Hans-Walter Rix, Peter Schneider, Thomas Erben, Klaus Meisenheimer, Christian Wolf, and Mischa Schirmer. "Galaxy-Galaxy Lensing Studies from COMBO-17." Proceedings of the International Astronomical Union 2004, IAUS225 (July 2004): 249–54. http://dx.doi.org/10.1017/s174392130500205x.

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36

Martinez, Hector J., Manuel E. Merchan, Carlos A. Valotto, and Diego G. Lambas. "Quasar‐Galaxy and AGN‐Galaxy Cross‐Correlations." Astrophysical Journal 514, no. 2 (April 1999): 558–62. http://dx.doi.org/10.1086/306973.

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Ebbels, Tim, Jean-Paul Kneib, and Richard Ellis. "Weak Galaxy-Galaxy Lensing in HST DATA." Symposium - International Astronomical Union 183 (1999): 247. http://dx.doi.org/10.1017/s0074180900132644.

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We expand on the work of Brainerd, Blandford & Smail (1996) (BBS), using a larger archival WFPC-2 dataset including many galaxy redshifts. It is clear from our data that the ellipticity distribution of images changes substantially with observed magnitude (figure 1, left) which is shown by simulations to be mainly the result of detection effects. We have detected a lensing signal, using a similar selection method to BBS and are also implementing a maximum likelihood method to constrain halo parameters. Using simulations, we show in figure 1 (right) that the signal is consistant with typical halo velocity dispersions of σ∗ ∼ 70–100 kms−1 However, the radial extent of the halos is less well constrained.

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Tissera, P. B., M. S. Alonso, D. G. Lambas, and G. Coldwell. "Triggering Star Formation by Galaxy-Galaxy Interactions." Symposium - International Astronomical Union 217 (2004): 434–35. http://dx.doi.org/10.1017/s0074180900198146.

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We analyzed the effects of having a close companion on the star formation activity of galaxies in the 8K galaxy pair catalog selected from the 2dFGRS. We found that, statistically, galaxies with rp < 25h−1 kpc and ΔV < 100km s−1 have enhanced star formation with respect to isolated galaxies with the same luminosity and redshift distribution. Our results suggest that the physical processes at work during tidal interactions can overcome the effects of environment, except in dense regions.

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Brainerd, Tereasa G. "MULTIPLE WEAK DEFLECTIONS IN GALAXY-GALAXY LENSING." Astrophysical Journal 713, no. 1 (March 24, 2010): 603–14. http://dx.doi.org/10.1088/0004-637x/713/1/603.

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40

Okazaki, Tadashi, and Yoshiaki Taniguchi. "Dwarf Galaxy Formation Induced by Galaxy Interactions." Astrophysical Journal 543, no. 1 (November 2000): 149–52. http://dx.doi.org/10.1086/317109.

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41

Blazek, Jonathan, Rachel Mandelbaum, Uroš Seljak, and Reiko Nakajima. "Separating intrinsic alignment and galaxy-galaxy lensing." Journal of Cosmology and Astroparticle Physics 2012, no. 05 (May 31, 2012): 041. http://dx.doi.org/10.1088/1475-7516/2012/05/041.

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Zacharegkas, G., C. Chang, J. Prat, S. Pandey, I. Ferrero, J. Blazek, B. Jain, et al. "Dark Energy Survey Year 3 results: galaxy–halo connection from galaxy–galaxy lensing." Monthly Notices of the Royal Astronomical Society 509, no. 3 (November 11, 2021): 3119–47. http://dx.doi.org/10.1093/mnras/stab3155.

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ABSTRACT Galaxy–galaxy lensing is a powerful probe of the connection between galaxies and their host dark matter haloes, which is important both for galaxy evolution and cosmology. We extend the measurement and modelling of the galaxy–galaxy lensing signal in the recent Dark Energy Survey Year 3 cosmology analysis to the highly non-linear scales (∼100 kpc). This extension enables us to study the galaxy–halo connection via a Halo Occupation Distribution (HOD) framework for the two lens samples used in the cosmology analysis: a luminous red galaxy sample (redmagic) and a magnitude-limited galaxy sample (maglim). We find that redmagic (maglim) galaxies typically live in dark matter haloes of mass log10(Mh/M⊙) ≈ 13.7 which is roughly constant over redshift (13.3−13.5 depending on redshift). We constrain these masses to ${\sim}15{{\ \rm per\ cent}}$, approximately 1.5 times improvement over the previous work. We also constrain the linear galaxy bias more than five times better than what is inferred by the cosmological scales only. We find the satellite fraction for redmagic (maglim) to be ∼0.1−0.2 (0.1−0.3) with no clear trend in redshift. Our constraints on these halo properties are broadly consistent with other available estimates from previous work, large-scale constraints, and simulations. The framework built in this paper will be used for future HOD studies with other galaxy samples and extensions for cosmological analyses.

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Cacciato, Marcello, Frank C. van den Bosch, Surhud More, Ran Li, H. J. Mo, and Xiaohu Yang. "Galaxy clustering and galaxy-galaxy lensing: a promising union to constrain cosmological parameters." Monthly Notices of the Royal Astronomical Society 394, no. 2 (April 1, 2009): 929–46. http://dx.doi.org/10.1111/j.1365-2966.2008.14362.x.

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Mandelbaum, Rachel, Uroš Seljak, Richard J. Cool, Michael Blanton, Christopher M. Hirata, and Jonathan Brinkmann. "Density profiles of galaxy groups and clusters from SDSS galaxy-galaxy weak lensing." Monthly Notices of the Royal Astronomical Society 372, no. 2 (October 21, 2006): 758–76. http://dx.doi.org/10.1111/j.1365-2966.2006.10906.x.

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Chaves-Montero, Jonás, and Andrew Hearin. "Surrogate modelling the Baryonic Universe – I. The colour of star formation." Monthly Notices of the Royal Astronomical Society 495, no. 2 (May 16, 2020): 2088–104. http://dx.doi.org/10.1093/mnras/staa1230.

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ABSTRACT The spectral energy distribution of a galaxy emerges from the complex interplay of many physical ingredients, including its star formation history (SFH), metallicity evolution, and dust properties. Using galaxpy, a new galaxy spectral prediction tool, and SFHs predicted by the empirical model universemachine and the cosmological hydrodynamical simulation IllustrisTNG, we isolate the influence of SFH on optical and near-infrared colours from 320 to 1080 Å at z = 0. By carrying out a principal component analysis, we show that physically motivated SFH variations modify galaxy colours along a single direction in colour space: the SFH-direction. We find that the projection of a galaxy’s present-day colours on to the SFH-direction is almost completely regulated by the fraction of stellar mass that the galaxy formed over the last billion years. Together with cosmic downsizing, this results in galaxies becoming redder as their host halo mass increases. We additionally study the change in galaxy colours due to variations in metallicity, dust attenuation, and nebular emission lines, finding that these properties vary broad-band colours along distinct directions in colour space relative to the SFH-direction. Finally, we show that the colours of low-redshift Sloan Digital Sky Survey galaxies span an ellipsoid with significant extent along two independent dimensions, and that the SFH-direction is well-aligned with the major axis of this ellipsoid. Our analysis supports the conclusion that variations in SFH are the dominant influence on present-day galaxy colours, and that the nature of this influence is strikingly simple.

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Meno, Frank M., and Kassem Awada. "Galaxy Evolution." Physics Essays 12, no. 1 (March 1999): 106–14. http://dx.doi.org/10.4006/1.3025353.

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Hopkins, Andrew. "Galaxy Metabolism." Publications of the Astronomical Society of Australia 27, no. 3 (2010): 233. http://dx.doi.org/10.1071/as10012.

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‘Galaxy Metabolism' was the second in the annual ‘Southern Cross Astrophysics Conference Series’ (http://www.aao.gov.au/AAO/southerncross/), supported by the Anglo-Australian Observatory and the Australia Telescope National Facility. It was held at the Australian National Maritime Museum in Darling Harbour, Sydney, from 22 to 26 June 2009, and was attended by 91 delegates from around the world.Over the past decade, both the star formation history and stellar mass density in galaxies spanning most of cosmic history have been well constrained. This provides the backdrop and framework within which many detailed investigations of galaxy growth are now placed. The mass-dependent and environment-dependent evolution of galaxies over cosmic history is now the focus of several surveys. Many studies are also exploring the role of gas infall and outflow in driving galaxy evolution, and the connection of these processes to massive star formation within galaxies.The aims of ‘Galaxy Metabolism’ were to bring together the global constraints on galaxy evolution, at both low and high redshift, with detailed studies of well-resolved systems, to define a clear picture of our understanding of galaxy metabolism: How do the processes of ingestion (infall), digestion (ISM physics, star formation) and excretion (outflow) govern the global properties of galaxies; how do these change over a galaxy's lifetime; and are the constraints from nearby well resolved studies consistent with those from large population surveys at low and high redshift?The conference was a great success, with an extensive variety of topics covered spanning many aspects of galaxy evolution, and brought together eloquently in a comprehensive conference summary by Warrick Couch. The four papers by De Lucia (2010), Cole (2010), Vlajić (2010) and Stocke et al. (2010) presented in this special collection of PASA are just a sampling of the depth and variety of the resentations given during the conference.

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Shiga, David. "Ghostly Galaxy." Science News 167, no. 9 (February 26, 2005): 131. http://dx.doi.org/10.2307/4015891.

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Dunlop, James. "Galaxy connections." Nature 459, no. 7243 (May 2009): 43–44. http://dx.doi.org/10.1038/459043b.

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Brent Tully, R. "GALAXY GROUPS." Astronomical Journal 149, no. 2 (January 15, 2015): 54. http://dx.doi.org/10.1088/0004-6256/149/2/54.

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