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Готові списки джерел за темами / Galaxies : à haute redshift / Статті в журналах

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Статті в журналах з теми "Galaxies : à haute redshift"

Автор: Grafiati

Опубліковано: 23 вересня 2022

Оновлено: 31 липня 2025

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1

Mickaelian, A. M., S. K. Balayan, and S. A. Hakopian. "The Byurakan-IRAS Galaxy (BIG) Sample: The Redshift Survey." International Astronomical Union Colloquium 184 (2002): 217–19. http://dx.doi.org/10.1017/s0252921100030724.

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AbstractThe Byurakan-IRAS Galaxy (BIG) sample (1967 galaxies) is based on optical identifications of IRAS PSC sources at δ>+61° and |b| >15° (FBS area). A redshift survey for brighter objects (B<18m) is being carried out with the Byurakan Observatory 2.6m, Special Observatory 6m, and Observatoire de Haute-Provence 1.93m telescopes. 213 objects have been observed, and redshifts in the range 0.008-0.173 have been measured. For this subsample, 15% of the objects are AGNs, and 15% are LIGs and ULIGs.

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2

Mickaelian, A. M. "Investigation of the Local Universe by Means of IRAS Galaxies." Symposium - International Astronomical Union 204 (2001): 69. http://dx.doi.org/10.1017/s0074180900225904.

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The Byurakan-IRAS galaxy (BIG) sample is based on optical identifications of IRAS PSC sources (Beichman, C. A. et al., eds. 1988, Infrared Astronomical Satellite (IRAS) Catalogs and Atlases: The Point Source Catalog, NASA RP–1190, Washington, DC). It makes use of the IR colours, DSS images, and the First Byurakan Spectral Survey (Markarian, B. E. et al. 1989, Commun. Special Astrophys. Obs., 62, 5).All IRAS sources in the region +61° < δ < 90° at high galactic latitudes (|b| >15°) in an area of 1487 deg2 have been revealed up to the limit of the IRAS survey. The BIG sample (Mickaelian

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3

Mickaelian, Areg M. "Galaxy Evolution Traced by Multiple Galaxies from the BIG Sample." Proceedings of the International Astronomical Union 2, S235 (2006): 225. http://dx.doi.org/10.1017/s1743921306006314.

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AbstractOptical identifications of all IRAS PSC sources at high galactic latitudes by means of the First Byurakan Survey (FBS) in the area with +61° < δ < +90° at galactic latitudes |b|>15° have been carried out with a total surface of 1487 deg2. 1577 sources have been optically identified, 1178 sources corresponding to galaxies. The BIG sample (Byurakan-IRAS Galaxies) was constructed of 1178 newly identified galaxies and 789 other IRAS galaxies in the same area, known before, altogether 1967 galaxies. Studies of the BIG objects include: spectroscopic follow-up for the brighter (<1

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4

Barger, Amy. "High-Redshift Galaxies." Symposium - International Astronomical Union 216 (2005): 309–24. http://dx.doi.org/10.1017/s0074180900196743.

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Mapping the history of star formation requires combining observations at many wavelengths. The most dramatic episodes of star formation occurred in high-redshift (z > 1) galaxies obscured by dust. These galaxies can be seen at submillimeter wavelengths. While these episodes clearly constitute much of the star formation in the universe, we still do not know the redshift distribution. Although progess has been made in determining the nature of the brightest members of the submillimeter population, these galaxies comprise only a tiny fraction of the submillimeter extragalactic background light

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5

Bian, Fuyan, Lisa J. Kewley, Brent Groves, and Michael A. Dopita. "What drives the redshift evolution of strong emission line ratios?" Monthly Notices of the Royal Astronomical Society 493, no. 1 (2020): 580–85. http://dx.doi.org/10.1093/mnras/staa259.

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ABSTRACT We study the physical mechanisms that cause the offset between low-redshift and high-redshift galaxies on the [O iii] λ5007/H β versus [N ii] λ6584/H α ‘Baldwin, Phillips & Terlevich’ (BPT) diagram using a sample of local analogues of high-redshift galaxies. These high-redshift analogue galaxies are selected from the Sloan Digital Sky Survey. Located in the same region on the BPT diagram as the ultraviolet selected galaxies at z ∼ 2, these high-redshift analogue galaxies provide an ideal local benchmark to study the offset between the local and high-redshift galaxies on the BPT di

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6

Li, I. H., H. K. C. Yee, B. C. Hsieh, D. G. Gilbank, and M. D. Gladders. "The Evolution of Galaxies and Groups in Cluster Environments at 0.3 < z < 0.6." Proceedings of the International Astronomical Union 2, S235 (2006): 220. http://dx.doi.org/10.1017/s1743921306006260.

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We investigate the dependence of galaxy populations on environment. Our samples are selected from the follow-up of Red-Sequence Cluster Survey (RCS) catalogs using wide-field BVRz' imaging for 60 intermediate redshift (0.3 < z < 0.6) clusters. Galaxy redshifts are estimated using an empirical photometric redshift technique with a training set of 3996 galaxies to z 1.4. To obtain photometric redshift probability density for each galaxy, we bootstrap the training set galaxies to estimate the fitting uncertainties and apply Monte-Carlo method to simulate galaxy magnitudes errors. In order t

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7

Mahdi, Hareth Saad. "The Bimodal Color Distribution of Galaxies at Redshift of z=0-0.15 from the Sloan Digital Sky Survey (SDSS)." Al-Mustansiriyah Journal of Science 30, no. 2 (2019): 52. http://dx.doi.org/10.23851/mjs.v30i2.574.

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This work aims to use the color distribution of galaxies to differentiate between blue and red galaxies. The photometric data of 300000 galaxies at redshift of z = 0 – 0.15 were collected from the Sloan Digital Sky Survey (SDSS). Three redshift ranges were considered for the purpose of this work: 100000 galaxies at z = 0-0.05, 100000 galaxies at z = 0.05-0.1 and 100000 galaxies at z = 0.1-0.15. The color distributions for all redshift ranges were determined. The results have clearly shown that the color distributions for all redshift ranges are bimodal. One of the two peaks corresponds to the

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8

Jaskot, Anne, and Sally Oey. "The Green Peas: Searching for LyC Emitters at Low Redshift." Proceedings of the International Astronomical Union 11, S319 (2015): 126. http://dx.doi.org/10.1017/s1743921315010054.

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AbstractThe escape fraction of Lyman continuum (LyC) radiation from galaxies remains one of the primary uncertainties in studies of reionization. However, few LyC-emitting galaxies are known. The recently identified, low-redshift “Green Pea” (GP) galaxies exhibit a number of similarities with high-redshift galaxies, and their optical emission lines suggest they may be some of the elusive LyC emitters. Recent HST COS and ACS observations of four GPs suggest further evidence for LyC escape and give new insights into the origins of Lyα and low-ionization UV lines in high-redshift galaxies. The Ly

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9

Bian, Fuyan, Lisa J. Kewley, Brent Groves, and Michael A. Dopita. "Local analogs of high-redshift galaxies: Metallicity calibrations at high-redshift." Proceedings of the International Astronomical Union 15, S352 (2019): 309–13. http://dx.doi.org/10.1017/s1743921320000800.

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AbstractWe study the metallicity calibrations in high-redshift galaxies using a sample of local analogs of high-redshift galaxies selected from the SDSS survey. Located in the same region on the BPT diagram as star-forming galaxies at z ∼ 2, these high-redshift analogs share the same ionized ISM conditions as high-redshift galaxies. We establish empirical metallicity calibrations between the direct gas-phase oxygen abundances and varieties of metallicity indicators in our local analogs using direct Te method. These new metallicity calibrations are the best means to measure the metallicity in h

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10

Yuan, Qi-Rong, Qiang-Qiang Dang, Peng-Fei Yan, et al. "Correlation of morphological fraction with redshift in galaxy clusters." Proceedings of the International Astronomical Union 10, H16 (2012): 136. http://dx.doi.org/10.1017/s1743921314004979.

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AbstractBased on 187 galaxy clusters identified from the photometric redshifts of galaxies in the Cosmic Evolution Survey (COSMOS) field(Wen & Han 2011), cluster galaxies brighter than MV = -20.5 are classified into four categories according to their best-fitting templates of the spectral energy distributions (SEDs) provided by Ilbert et al. (2009): early-type (including elliptical and lenticular) galaxies (E+S0), spiral galaxies (S), irregular galaxies (Irr), and starbursts (SB). The fractions of these four SED types are presented as the functions of redshift in Figure 1. Fraction of each

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11

Yoifoi, Ponlawat, and Wichean Kriwattanawong. "Galaxy evolution in different environments along redshift within the local universe z < 0.8." Journal of Physics: Conference Series 2145, no. 1 (2021): 012002. http://dx.doi.org/10.1088/1742-6596/2145/1/012002.

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Abstract This study presents the evolution of the galaxies in different matter density along redshift within the local universe. A sample of 702,352 galaxies was collected from the Sloan Digital Sky Survey (SDSS). Under the limitation of the spectroscopic data, the appropriate photometric redshift was used to represent the spectroscopic redshift in the range of 0.0 ≤ z ≤ 0.8. Number density of galaxies, galaxy’s colors, and star formation activities are considered to describe the evolution of galaxies. In summary, the number density is not clearly different although the Dec and RA of the sky a

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12

Giovanelli, Riccardo, and Martha P. Haynes. "Redshift Surveys of Galaxies." Annual Review of Astronomy and Astrophysics 29, no. 1 (1991): 499–541. http://dx.doi.org/10.1146/annurev.aa.29.090191.002435.

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13

McCarthy, Patrick J. "High Redshift Radio Galaxies." Annual Review of Astronomy and Astrophysics 31, no. 1 (1993): 639–88. http://dx.doi.org/10.1146/annurev.aa.31.090193.003231.

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14

Salvaterra, Ruben, Andrea Ferrara, and Pratika Dayal. "Simulating high-redshift galaxies." Monthly Notices of the Royal Astronomical Society 414, no. 2 (2011): 847–59. http://dx.doi.org/10.1111/j.1365-2966.2010.18155.x.

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15

Pelló, Roser, Daniel Schaerer, Johan Richard, et al. "High-redshift lensed galaxies." Proceedings of the International Astronomical Union 2, no. 14 (2006): 250. http://dx.doi.org/10.1017/s1743921307010320.

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16

Miley, George. "High-Redshift Radio Galaxies." Highlights of Astronomy 10 (1995): 543–46. http://dx.doi.org/10.1017/s1539299600011990.

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Radio galaxies are unique cosmological probes. As with radio-loud quasars, the presence of luminous radio continuum and optical line emission enable radio galaxies to be observed and recognized at large distances, up to z = 4.2. However, unlike the situation for most quasars, their optical emission can be spatially resolved from the ground and studied in detail.Progress in detecting distant radio galaxies has been rapid in recent years due to the use of CCDs and the exploitation of new selection criteria. Now, more than 60 radio galaxies are known with z > 2. More than half of these have be

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17

Meisenheimer, K., H. Hippelein, and M. Neeser. "High Redshift Radio Galaxies." Symposium - International Astronomical Union 175 (1996): 571–76. http://dx.doi.org/10.1017/s0074180900081894.

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One hundred years after G. Marconi recorded radio waves over a distance of more than 1000 m, the most sensitive radio telescopes are able to detect the radio emission from light travel distances at least 1.4 × 1023 times greater. The electromagnetic waves from these distant objects are red shifted by Δλ/λ = z > 4. It is not the mere distance of high redshift objects which is fascinating, but rather the fact that one looks back into the early history of the universe by observing them: Objects at a redshift of 4 shined at a time when the universe had reached only about 1/5 of its present age.

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18

Dunlop, James S. "High Redshift Radio Galaxies." Symposium - International Astronomical Union 168 (1996): 79–87. http://dx.doi.org/10.1017/s0074180900109957.

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The potentially important role of jet-cloud interactions in determining the appearance of high-redshift radio galaxies is discussed and investigated via new 3-dimensional simulations of off-axis jet-cloud collisions. The results indicate that the most powerful radio sources are likely to be observed during or shortly after a jet-cloud interaction, and that such interactions can explain both the radio structures and the spatial association between optical and radio light found in powerful radio galaxies at high redshift. It is argued that, due to the radio-power dependence of such complicating

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19

Hubertus, Angelina. "Lyman- Spectra shapes in high redshift and low redshift galaxies." Theoretical and Natural Science 10, no. 1 (2023): 241–46. http://dx.doi.org/10.54254/2753-8818/10/20230352.

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Lyman-alpha (Ly) photons were first predicted by Theodore Lyman in 1906 as part of his work on the hydrogen atom spectrum. The Ly transition occurs when an electron in a hydrogen atom falls from the second energy level to the ground state, releasing a photon with a wavelength of 121.6 nanometres. It was not until the 1960s that Ly photons were observed in astronomical sources, including galaxies and quasars. Since then, the Ly line has been recognized as a powerful probe of the intergalactic medium and the properties of galaxies, providing insights into the formation and evolution of structure

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20

Chisholm, J., S. Gazagnes, D. Schaerer, et al. "Accurately predicting the escape fraction of ionizing photons using rest-frame ultraviolet absorption lines." Astronomy & Astrophysics 616 (August 2018): A30. http://dx.doi.org/10.1051/0004-6361/201832758.

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The fraction of ionizing photons that escape high-redshift galaxies sensitively determines whether galaxies reionized the early Universe. However, this escape fraction cannot be measured from high-redshift galaxies because the opacity of the intergalactic medium is large at high redshifts. Without methods to measure the escape fraction of high-redshift galaxies indirectly, it is unlikely that we will know what reionized the Universe. Here, we analyze the far-ultraviolet (UV) H I (Lyman series) and low-ionization metal absorption lines of nine low-redshift, confirmed Lyman continuum emitting ga

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21

Susa, Hajime, and Masayuki Umemura. "A Simulation of Galaxy Formation by Radiation-SPH." Symposium - International Astronomical Union 208 (2003): 323–30. http://dx.doi.org/10.1017/s0074180900207274.

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We investigate galaxy formation with Radiation-SPH simulations in order to find the effects of ultraviolet background radiation field on the star formation in the forming galaxies. We find the ultraviolet background radiation field can delay the star formation in protogalactic clouds, especially at low redshift (z < 2). This result suggests that galaxies formed at lower redshift tend to be late type galaxies, and early type galaxies tend to be formed at higher redshift.

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22

Shamir, Lior. "An Empirical Consistent Redshift Bias: A Possible Direct Observation of Zwicky’s TL Theory." Particles 7, no. 3 (2024): 703–16. http://dx.doi.org/10.3390/particles7030041.

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Recent advancements have shown tensions between observations and our current understanding of the Universe. Such observations may include the H0 tension and massive galaxies at high redshift that are older than traditional galaxy formation models have predict. Since these observations are based on redshift as the primary distance indicator, a bias in the redshift may explain these tensions. While redshift follows an established model, when applied to astronomy it is based on the assumption that the rotational velocity of the Milky Way galaxy relative to the observed galaxies has a negligible e

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23

Chakraborty, Priyanka, Arnab Sarkar, Randall Smith, et al. "Unveiling the Cosmic Chemistry. II. “Direct” T _e-based Metallicity of Galaxies at 3 < z < 10 with JWST/NIRSpec." Astrophysical Journal 985, no. 1 (2025): 24. https://doi.org/10.3847/1538-4357/adc7b5.

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Abstract We report the detection of the [O iii] auroral line in 42 galaxies within the redshift range of 3 < z < 10. These galaxies were selected from publicly available JWST data releases, including the JADES and PRIMAL surveys, and observed using both the low-resolution PRISM/CLEAR configuration and medium-resolution gratings. The measured electron temperatures in the high-ionization regions of these galaxies range from T e ([O iii]) = 12,000 to 24,000 K, consistent with temperatures observed in local metal-poor galaxies and previous JWST studies. In 10 galaxies, we also detect the [O

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24

Shuntov, M., J. Pasquet, S. Arnouts, et al. "PhotoWeb redshift: boosting photometric redshift accuracy with large spectroscopic surveys." Astronomy & Astrophysics 636 (April 2020): A90. http://dx.doi.org/10.1051/0004-6361/201937382.

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Improving distance measurements in large imaging surveys is a major challenge to better reveal the distribution of galaxies on a large scale and to link galaxy properties with their environments. As recently shown, photometric redshifts can be efficiently combined with the cosmic web extracted from overlapping spectroscopic surveys to improve their accuracy. In this paper we apply a similar method using a new generation of photometric redshifts based on a convolution neural network (CNN). The CNN is trained on the SDSS images with the main galaxy sample (SDSS-MGS, r ≤ 17.8) and the GAMA spectr

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25

Arp, Halton. "Redshifts of New Galaxies." Symposium - International Astronomical Union 194 (1999): 347–55. http://dx.doi.org/10.1017/s007418090016228x.

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Observations increasingly demonstrate the spatial association of high redshift objects with larger, low redshift galaxies. These companion objects show a continuous range of physical properties - from very compact, high redshift quasars, through smaller active galaxies and finally to only slightly smaller companion galaxies of slightly higher redshift. The shift in energy distribution from high to low makes it clear that are seeing an empirical evolution from newly created to older, more normal galaxies.In order to account for the evolution of intrinsic redshift we must conclude that matter is

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26

Cramer, W. J., A. G. Noble, K. Massingill, et al. "A Large-scale Kinematic Study of Molecular Gas in High-z Cluster Galaxies: Evidence for High Levels of Kinematic Asymmetry." Astrophysical Journal 944, no. 2 (2023): 213. http://dx.doi.org/10.3847/1538-4357/acae96.

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Abstract We investigate the resolved kinematics of the molecular gas, as traced by the Atacama Large Millimeter/submillimeter Array in CO (2−1), of 25 cluster member galaxies across three different clusters at a redshift of z ∼ 1.6. This is the first large-scale analysis of the molecular gas kinematics of cluster galaxies at this redshift. By separately estimating the rotation curve of the approaching and receding sides of each galaxy via kinematic modeling, we quantify the difference in total circular velocity to characterize the overall kinematic asymmetry of each galaxy. 3/14 of the galaxie

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27

Chugunov, I. V., and A. A. Marchuk. "Decomposition of 138 galaxies at 0.1 < z < 2.2 with spiral structure." Publications of the Pulkovo Observatory 232 (March 2024): 8–28. http://dx.doi.org/10.31725/0367-7966-2024-232-8-28.

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Various problems concerning the origin and evolution of spiral arms in galaxies are still remain unsettled. Also, only few studies are devoted to the parameters of the spiral structure in distant galaxies. To investigate this, we have performed decomposition with spiral arms of 138 distant galaxies from COSMOS and CEERS surveys, located at redshift 0.1 < z < 2.2 (up to 10.5 Gyr ago). For all 9 galaxies from CEERS, multi-band images are utilized. As a result, different parameters dependence on redshift and wavelength are studied. In particular, we confirm that pitch angle of spiral arms i

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28

Malhotra, Sangeeta, та James E. Rhoads. "High-redshift Lyman-α galaxies". Proceedings of the International Astronomical Union 2, № 14 (2006): 254. http://dx.doi.org/10.1017/s1743921307010368.

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A strong Lyman-α line enables relatively easy detection of high redshift galaxies. Lyman-α galaxies are now known from z = 3 to 6.6. No evolution is discerned in the Lyman-α line luminosity function in this redshift range. This implies that the intergalactic medium at z = 6 is at least 50% ionized over more than 50% of the volume. Recent continuum detections of these galaxies from HST, MMT and Spitzer are now allowing us to address questions about the nature of these Lyman-α emitters, their stellar populations and ages. We find that by and large the Lyman-α galaxies are young galaxies dominate

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29

Bian, Fuyan, Lisa J. Kewley, Michael A. Dopita, and Stephanie Juneau. "Local analogs of high-redshift galaxies: Interstellar medium conditions." Proceedings of the International Astronomical Union 11, S321 (2016): 333–35. http://dx.doi.org/10.1017/s1743921316009261.

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AbstractLocal analog galaxies play an important role in understanding the properties of high-redshift galaxies. We present a method to select a type of local analog that closely resembles the ionized interstellar medium conditions in high-redshift galaxies. These galaxies are selected based on their locations in the [O III]/Hβ versus [N II]/Hα nebular emission-line diagnostic diagram. The ionization parameters and electron densities in these analogs are comparable to those in z ≃ 2 − 3 galaxies, but higher than those in normal SDSS galaxies by ≃ 0.6 dex and ≃ 0.9 dex, respectively. We find tha

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30

Wilkinson, Aaron, Omar Almaini, Vivienne Wild, et al. "From starburst to quiescence: post-starburst galaxies and their large-scale clustering over cosmic time." Monthly Notices of the Royal Astronomical Society 504, no. 3 (2021): 4533–50. http://dx.doi.org/10.1093/mnras/stab965.

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ABSTRACT We present the first study of the large-scale clustering of post-starburst (PSB) galaxies in the high-redshift Universe (0.5 &lt; z &lt; 3.0). We select ∼4000 PSB galaxies photometrically, the largest high-redshift sample of this kind, from two deep large-scale near-infrared surveys: the UKIDSS Ultra Deep Survey Data Release 11 and the Cosmic Evolution Survey. Using angular cross-correlation techniques, we estimate the halo masses for this large sample of PSB galaxies and compare them with quiescent and star-forming galaxies selected in the same fields. We find that low-mass,

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31

Lan, Ting-Wen, R. Tojeiro, E. Armengaud, et al. "The DESI Survey Validation: Results from Visual Inspection of Bright Galaxies, Luminous Red Galaxies, and Emission-line Galaxies." Astrophysical Journal 943, no. 1 (2023): 68. http://dx.doi.org/10.3847/1538-4357/aca5fa.

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Abstract The Dark Energy Spectroscopic Instrument (DESI) Survey has obtained a set of spectroscopic measurements of galaxies to validate the final survey design and target selections. To assist in these tasks, we visually inspect DESI spectra of approximately 2500 bright galaxies, 3500 luminous red galaxies (LRGs), and 10,000 emission-line galaxies (ELGs) to obtain robust redshift identifications. We then utilize the visually inspected redshift information to characterize the performance of the DESI operation. Based on the visual inspection (VI) catalogs, our results show that the final survey

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32

Toffano, Mattia, Michela Mapelli, Nicola Giacobbo, M. Celeste Artale, and Giancarlo Ghirlanda. "The host galaxies of double compact objects across cosmic time." Monthly Notices of the Royal Astronomical Society 489, no. 4 (2019): 4622–31. http://dx.doi.org/10.1093/mnras/stz2415.

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ABSTRACT We explore the host galaxies of compact-object binaries (black hole–black hole binaries, BHBs; neutron star–black hole binaries, NSBHs; double–neutron stars; DNSs) across cosmic time, by means of population-synthesis simulations combined with the Illustris cosmological simulation. At high redshift (z ≳ 4), the host galaxies of BHBs, NSBHs, and DNSs are very similar and are predominantly low-mass galaxies (stellar mass M < 1011 M⊙). If z ≳ 4, most compact objects form and merge in the same galaxy, with a short delay time. At low redshift (z ≤ 2), the host galaxy populations of DNSs

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33

Byrd, Gene G., and Mauri J. Valtonen. "Redshift Asymmetries and the Missing Mass." Symposium - International Astronomical Union 124 (1987): 503–6. http://dx.doi.org/10.1017/s0074180900159455.

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We study the existence of missing mass in the outermost regions of galaxies not accessible to study by rotation curve methods. We consider binary galaxies, groups and clusters of galaxies. Arp has previously explained redshift asymmetries in pairs or groups with “non-Doppler redshifts”. Instead, we propose the asymmetries indicate contamination by optical pairs or by members which are not gravitationally bound to the group or pair. The group samples which are commonly used to justify very high missing mass values in spiral galaxies (>> the mass detected by rotation curves) also exhibit s

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34

A Norman, Colin. "Star Formation at High Redshift." Australian Journal of Physics 45, no. 4 (1992): 389. http://dx.doi.org/10.1071/ph920389.

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Анотація:

The observations relevant to star formation at high redshift are reviewed including radio galaxies, quasars, IRAS objects, and QSO emission and absorption line regions. Low redshift counterparts associated with starburst galaxies are discussed. The relation of galaxy formation, starbursts, and active galaxies and quasars is briefly reviewed. The role of feedback in galaxy formation and massive star formation is briefly analysed.

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35

Pharo, John, Yicheng Guo, Guillermo Barro Calvo, et al. "The Dwarf Galaxy Population at z ∼ 0.7: A Catalog of Emission Lines and Redshifts from Deep Keck Observations." Astrophysical Journal Supplement Series 261, no. 2 (2022): 12. http://dx.doi.org/10.3847/1538-4365/ac6cdf.

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Abstract We present a catalog of spectroscopically measured redshifts over 0 < z < 2 and emission-line fluxes for 1440 galaxies. The majority (∼65%) of the galaxies come from the HALO7D survey, with the remainder from the DEEPwinds program. This catalog includes redshifts for 646 dwarf galaxies with log ( M ⋆ / M ⊙ ) < 9.5 . Eight-hundred and ten catalog galaxies did not have previously published spectroscopic redshifts, including 454 dwarf galaxies. HALO7D used the DEIMOS spectrograph on the Keck II telescope to take very deep (up to 32 hr exposure, with a median of ∼7 hr) optical sp

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36

Snellen, Ignas, Malcolm Bremer, Richard Schilizzi, George Miley, and Rob Van Ojik. "The R-Band Hubble Diagram for GPS Galaxies." Symposium - International Astronomical Union 175 (1996): 585–87. http://dx.doi.org/10.1017/s0074180900081936.

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The Hubble diagram of GPS galaxies has a low dispersion and a steep slope compared with that for 3C galaxies. The relative faintness of GPS galaxies at high redshift may be due to the absence of the aligned optical/uv component seen in high redshift 3C galaxies. The GPS Hubble relation is too steep to fit with evolution models for passively evolving ellipticals. This could be caused by the dynamical evolution of the GPS galaxies.

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37

Wen, Z. L., and J. L. Han. "Photometric redshifts for galaxies in the Subaru Hyper Suprime-Cam and unWISE and a catalogue of identified clusters of galaxies." Monthly Notices of the Royal Astronomical Society 500, no. 1 (2020): 1003–17. http://dx.doi.org/10.1093/mnras/staa3308.

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ABSTRACT We first present a catalogue of photometric redshifts for 14.68 million galaxies derived from the 7-band photometric data of Hyper Suprime-Cam Subaru Strategic Program and the Wide-field Infrared Survey Explorer using the nearest-neighbour algorithm. The redshift uncertainty is about 0.024 for galaxies of z ≤ 0.7, and steadily increases with redshift to about 0.11 at z ∼ 2. From such a large data set, we identify 21 661 clusters of galaxies, among which 5537 clusters have redshifts z &gt; 1 and 642 clusters have z &gt; 1.5, significantly enlarging the high redshift sample of g

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38

Malla, Janak Ratna, Walter Saurer, and Binil Aryal. "Study of Substructures in SDSS Supercluster S[173+014+0082]." Journal of Nepal Physical Society 8, no. 1 (2022): 35–38. http://dx.doi.org/10.3126/jnphyssoc.v8i1.48283.

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We present magnitude, color, redshift and number density distributions of 1302 galaxies in the supercluster S[173+014+0082]. Our aim is to identify substructures and study their redshift maps. The visual magnitude distribution suggests that the supercluster is dynamically unstable. We found 3 substructures in the supercluster region having mean redshift 0.083, 0.085 and 0.090. An empirical relation be-tween the number of galaxies in the substructures and their mean redshift is observed.

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39

Misquitta, Persis, Micah Bowles, Andreas Eckart, et al. "Interactions among intermediate redshift galaxies." Astronomy & Astrophysics 639 (July 2020): A30. http://dx.doi.org/10.1051/0004-6361/201937009.

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We present the properties of the central supermassive black holes and the host galaxies of the interacting object SDSS J134420.86+663717.8. We obtained optical long slit spectroscopy data from the Large Binocular Telescope using the Multi Object Double Spectrograph. Analysing the spectra revealed several strong broad and narrow emission lines of ionised gas in the nuclear region of one galaxy, whereas only narrow emission lines were visible for the second galaxy. The optical spectra were used to plot diagnostic diagrams, deduce rotation curves of the two galaxies, and calculate the masses of t

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40

Pettini, Max. "Disk Galaxies at High Redshift?" Proceedings of the International Astronomical Union 4, S254 (2008): 21–32. http://dx.doi.org/10.1017/s1743921308027348.

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AbstractThe successful implementation of integral field near-infrared spectrographs fed by adaptive optics is providing unprecedented views of gas motions within galaxies at redshifts z = 2 − 3, when the universe was forming stars at its peak rate. A complex picture of galaxy kinematics is emerging, with inflows, rotation within sometimes extended and nearly always thick disks, mergers, and galaxy-wide outflows all contributing to the variety of patterns seen. On the computational side, simulations of galaxy formation have reached a level of sophistication which can not only reproduce many of

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41

Pettini, Max, David L. King, Linda J. Smith, and Richard W. Hunstead. "Dust in High‐Redshift Galaxies." Astrophysical Journal 478, no. 2 (1997): 536–41. http://dx.doi.org/10.1086/303826.

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42

Pelló, R., D. Schaerer, J. Richard, J. F. Le Borgne, and J. P. Kneib. "Very High-Redshift Lensed Galaxies." Proceedings of the International Astronomical Union 2004, IAUS225 (2004): 373–86. http://dx.doi.org/10.1017/s1743921305002188.

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43

Scarpa, R., R. Falomo, and J. E. Pesce. "Redshift of southern radio galaxies." Astronomy and Astrophysics Supplement Series 116, no. 2 (1996): 295–300. http://dx.doi.org/10.1051/aas:1996115.

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44

Hwang, Ho Seong, Jihye Shin, and Hyunmi Song. "Evolution of star formation rate–density relation over cosmic time in a simulated universe: the observed reversal reproduced." Monthly Notices of the Royal Astronomical Society 489, no. 1 (2019): 339–48. http://dx.doi.org/10.1093/mnras/stz2136.

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ABSTRACT We use the IllustrisTNG cosmological hydrodynamical simulation to study the evolution of star formation rate (SFR)–density relation over cosmic time. We construct several samples of galaxies at different redshifts from z = 2.0 to z = 0.0, which have the same comoving number density. The SFR of galaxies decreases with local density at z = 0.0, but its dependence on local density becomes weaker with redshift. At z ≳ 1.0, the SFR of galaxies increases with local density (reversal of the SFR–density relation), and its dependence becomes stronger with redshift. This change of SFR–density r

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45

Kong, Xu, Jianhui Lian, Yulong Gao, et al. "Dwarf galaxies at low and high redshift." Proceedings of the International Astronomical Union 14, S344 (2018): 437–45. http://dx.doi.org/10.1017/s174392131800652x.

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AbstractThe overwhelming majority of galaxies in the Universe are dwarf galaxies. But although they are important components in understanding galaxy evolution, these systems are typically too faint to be observed at high redshifts. However, we are able to obtain an unobscured view of early star formation and chemical enrichment in these galaxies at low redshift and low-redshift analogs at high redshift. In this talk, I will review the mass-metallicity relation, the mass-star formation rate relation of galaxies, the classifications of dwarf galaxies, and the importance of dwarf galaxies for bot

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46

Bunker, Andrew J. "Stellar populations in the highest redshift galaxies." Proceedings of the International Astronomical Union 11, A29B (2015): 197–98. http://dx.doi.org/10.1017/s1743921316004877.

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AbstractI discuss stellar populations in galaxies at high redshift (z > 6), in particular the blue rest-frame UV colours which have been detected in recent years through near-IR imaging with HST. These spectral slopes of β < −2 are much more blue than star-forming galaxies at lower redshift, and may suggest less dust obscuration, lower metallicity or perhaps a different initial mass function. I describe current work on the luminosity function of high redshift star- forming galaxies, the evolution of the fraction of strong Lyman-α emitters in this population, and the contribution of the i

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47

Suess, Katherine A., Mariska Kriek, Rachel Bezanson, et al. "SQuIGGL⃗E : Studying Quenching in Intermediate-z Galaxies—Gas, AnguL⃗ar Momentum, and Evolution." Astrophysical Journal 926, no. 1 (2022): 89. http://dx.doi.org/10.3847/1538-4357/ac404a.

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Abstract We describe the Studying Quenching in Intermediate-z Galaxies: Gas, angu L → ar momentum, and Evolution ( SQuIGG L ⃗ E ) survey of intermediate-redshift post-starburst galaxies. We leverage the large sky coverage of the Sloan Digital Sky Survey to select ∼ 1300 recently quenched galaxies at 0.5 < z ≤ 0.9 based on their unique spectral shapes. These bright, intermediate-redshift galaxies are ideal laboratories to study the physics responsible for the rapid quenching of star formation: they are distant enough to be useful analogs for high-redshift quenching galaxies, but low enough r

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48

Daly, Ruth A., and Erick J. Guerra. "FRIIb Radio Galaxies, Cosmology, and Quintessence." Symposium - International Astronomical Union 201 (2005): 264–67. http://dx.doi.org/10.1017/s0074180900216343.

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Анотація:

FRIIb radio galaxies can be used as modified standard yardsticks to determine global cosmological parameters; the method is analogous to the use of supernovae type Ia as modified standard candles. FRIIb radio galaxies are observed to very high-redshift; the sources discussed here are fairly evenly distributed in redshift, with redshifts between zero and two. The sources can be used to determine the coordinate distance to high-redshift sources, and thus can constrain global cosmological parameters (just like the use of supernova type Ia to determine the coordinate distance, or luminosity distan

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49

Singal, J., G. Silverman, E. Jones, T. Do, B. Boscoe, and Y. Wan. "Machine Learning Classification to Identify Catastrophic Outlier Photometric Redshift Estimates." Astrophysical Journal 928, no. 1 (2022): 6. http://dx.doi.org/10.3847/1538-4357/ac53b5.

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Abstract We present results of using a basic binary classification neural network model to identify likely catastrophic outlier photometric redshift estimates of individual galaxies, based only on the galaxies’ measured photometric band magnitude values. We find that a simple implementation of this classification can identify a significant fraction of galaxies with catastrophic outlier photometric redshift estimates while falsely categorizing only a much smaller fraction of non-outliers. These methods have the potential to reduce the errors introduced into science analyses by catastrophic outl

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50

Pannella, M., D. Elbaz, and E. Daddi. "GOODS-Herschel: Dust attenuation up to z∼4." Proceedings of the International Astronomical Union 8, S292 (2012): 289. http://dx.doi.org/10.1017/s1743921313001439.

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AbstractWe quantitatively explore in a unbiased way the evolution of dust attenuation up to z ≈ 4 as a function of galaxy properties. We have used one of the deepest datasets available at present, in the GOODS-N field, to select a star forming galaxy sample and robustly measure galaxy redshifts, star formation rates, stellar masses and UV restframe properties. Our main results can be summarized as follows: i) we confirm that galaxy stellar mass is a main driver of UV dust attenuation in star forming galaxies: more massive galaxies are more dust attenuated than less massive ones; ii) strikingly

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