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Статті в журналах з теми "Tully-Fisher relation"

Автор: Grafiati

Опубліковано: 14 березня 2023

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1

Tully, Richard. "Tully-Fisher relation." Scholarpedia 2, no. 12 (2007): 4485. http://dx.doi.org/10.4249/scholarpedia.4485.

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2

M. ALI, AKRAM. "TULLY - FISHER RELATION PROOFING." Journal of University of Anbar for Pure Science 3, no. 3 (2009): 177–83. http://dx.doi.org/10.37652/juaps.2009.15642.

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3

Gurovich, Sebastián, Stacy S. McGaugh, Ken C. Freeman, Helmut Jerjen, Lister Staveley-Smith, and W. J. G. De Blok. "The Baryonic Tully–Fisher Relation." Publications of the Astronomical Society of Australia 21, no. 4 (2004): 412–14. http://dx.doi.org/10.1071/as04038.

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Анотація:

AbstractWe validate the baryonic Tully–Fisher (TF) relation by exploring the Tully–Fisher (TF) and BTF properties of optically and Hi-selected disk galaxies. The data includes galaxies from Sakai et al. (2000) calibrator sample, McGaugh et al. (2000: M2000) I-band sample, and 18 newly acquired Hi-selected field dwarf galaxies observed with the ANU 2.3-m telescope and the ATNF Parkes telescope (Gurovich 2005a).As in M2000, we re-cast the TF and BTF relations as relationships between baryon mass and W20. First we report some numerical errors in M2000. Then, we calculate weighted bi-variate linear fits to the data, and finally we compare the fits of the intrinsically fainter dwarfs with the brighter galaxies of Sakai et al. (2000). With regards to the local calibrator disk galaxies of Sakai et al. (2000), our results suggest that the BTF relation is indeed tighter than the TF relation and that the slopes of the BTF relations are statistically flatter than the equivalent TF relations. Further, for the fainter galaxies which include the I-band M2000 and Hi-selected galaxies of Gurovich's sample, we calculate a break from a simple power law model because of what appears to be real cosmic scatter. Not withstanding this point, the BTF models are marginally better models than the equivalent TF ones with slightly smaller Χred2 values.

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4

McGaugh, S. S., J. M. Schombert, G. D. Bothun, and W. J. G. de Blok. "The Baryonic Tully-Fisher Relation." Astrophysical Journal 533, no. 2 (2000): L99—L102. http://dx.doi.org/10.1086/312628.

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5

Meyer, Martin J., Martin A. Zwaan, Rachel L. Webster, and Stephen E. Schneider. "Tully-Fisher Relations from an HI-Selected Sample." Symposium - International Astronomical Union 220 (2004): 411–12. http://dx.doi.org/10.1017/s0074180900183731.

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Анотація:

The Tully-Fisher relation is of interest because of its use as a secondary distance measure and the constraints it places on the physics of rotationally supported galaxies. We use data from the HI Parkes All-Sky Survey Catalogue to study and apply the Tully-Fisher relation on a sample of galaxies selected on their HI properties. the issues of third parameter dependencies and intrinsic scatter of the Tully-Fisher relation are investigated.

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6

de Oliveira, Claudia Mendes, Sergio Torres-Flores, Philippe Amram, Henri Plana, and Benoit Epinat. "3D Studies of Galaxies in Compact Groups." Proceedings of the International Astronomical Union 10, S309 (2014): 175–77. http://dx.doi.org/10.1017/s1743921314009612.

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Анотація:

AbstractFabry-Perot data of compact group galaxies have been used to show that the Tully-Fisher relation in any photometric band, for galaxies with vmax > 100 km/s, is very similar to that for galaxies in other less dense environments. In the low-luminosity end, however, a few compact group galaxies fall above the relation apparently because they are too bright for their mass. Here we show that if the mass is properly computed from spectral energy distribution fitting or mass modelling, for the low-luminosity galaxies, their positions in the stellar-mass or baryonic Tully-Fisher relation are what is expected for a normal Tully-Fisher relation and the outlying positions observed in the B and K Tully-Fisher relation could be explained by brightening of the low-luminosity interacting galaxies due to strong star formation or AGN activity.

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7

Pfenniger, D., and Y. Revaz. "The Baryonic Tully-Fisher relation revisited." Astronomy & Astrophysics 431, no. 2 (2005): 511–16. http://dx.doi.org/10.1051/0004-6361:20041660.

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8

Andersen, David R., and Matthew A. Bershady. "A Face-on Tully-Fisher Relation." Astrophysical Journal 599, no. 2 (2003): L79—L82. http://dx.doi.org/10.1086/381292.

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9

Ferrero, Ismael, and Mario G. Abadi. "Redshift evolution of Tully-Fisher relation." Proceedings of the International Astronomical Union 11, S321 (2016): 126. http://dx.doi.org/10.1017/s1743921316009054.

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Анотація:

AbstractUsing the eagle cosmological simulation of galaxy formation we test the ability of the ΛCDM cosmological model to reproduce the Tully-Fisher relation (TFR) and its redshift evolution. We find that our simulated galaxies follow a TFR that is in good agreement with observed results up to z = 1, indicating no evolution in the slope and a weak decrease in the zero-point.

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10

Mould, Jeremy, Mingsheng Han, and Greg Bothun. "Nonlinearity of the Tully-Fisher relation." Astrophysical Journal 347 (December 1989): 112. http://dx.doi.org/10.1086/168101.

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11

Metevier, Anne J., and David C. Koo. "The Tully-Fisher Relation in Cl0024+1654 at z=0.4." Symposium - International Astronomical Union 220 (2004): 415–16. http://dx.doi.org/10.1017/s0074180900183755.

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Анотація:

We present the Tully-Fisher relation in cluster Cl0024+1654 at z=0.4. We find that our sample of 15 distant cluster members are ⋐ 0.5 mag overluminous as compared to local galaxies, and they exhibit slightly more Tully-Fisher scatter. This scatter is correlated with galaxy colours and sizes such that the smallest and bluest Cl0024 members in our sample are most overluminous.

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12

De Rossi, María E., Patricia B. Tissera, and Susana E. Pedrosa. "The Tully-Fisher Relation in Numerical Simulations of Structure Formation." Proceedings of the International Astronomical Union 5, S262 (2009): 327–28. http://dx.doi.org/10.1017/s1743921310003078.

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Анотація:

AbstractThe Tully-Fisher Relation (TFR) is of fundamental importance for galaxy formation as it provides information about the relation between the baryonic content of galaxies and the depth of their dark halos potential wells. In recent years, it has been possible to study this relation at different redshifts. However, there are still controversies about its origin and evolution. In this work, we try to address the origin of the Tully-Fisher Relation by employing cosmological hydrodynamical simulations.

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13

Böhm, A., B. L. Ziegler, R. P. Saglia, et al. "The Tully-Fisher relation at intermediate redshift." Astronomy & Astrophysics 420, no. 1 (2004): 97–114. http://dx.doi.org/10.1051/0004-6361:20034256.

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14

Persic, M., and P. Salucci. "Non-linearity of the Tully-Fisher relation." Monthly Notices of the Royal Astronomical Society 248, no. 2 (1991): 325–27. http://dx.doi.org/10.1093/mnras/248.2.325.

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15

Neistein, Eyal, Dan Maoz, Hans-Walter Rix, and John L. Tonry. "A Tully-Fisher Relation for S0 Galaxies." Astronomical Journal 117, no. 6 (1999): 2666–75. http://dx.doi.org/10.1086/300869.

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16

Biviano, A., G. Giuricin, F. Mardirossian, and M. Mezzetti. "The Tully-Fisher relation in different environments." Astrophysical Journal Supplement Series 74 (October 1990): 325. http://dx.doi.org/10.1086/191502.

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17

Yegorova, I., and P. Salucci. "The Tully-Fisher relation of spiral galaxies." Proceedings of the International Astronomical Union 1, no. C198 (2005): 267–68. http://dx.doi.org/10.1017/s174392130500390x.

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18

Giraud, E. "Distance Moduli from the Tully-Fisher Relation." Symposium - International Astronomical Union 124 (1987): 199–205. http://dx.doi.org/10.1017/s0074180900159157.

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Анотація:

When the Bottinelli et al. version of the Tully-Fisher relation is applied to derive distances, and when the observed parameters are used to predict the Malmquist bias at a given distance, the observed variation of the Hubble ratio as a function of kinematic distance is about 2.5 times the predicted variation.

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19

Makarov, D. I., N. A. Zaitseva, and D. V. Bizyaev. "The Tully–Fisher relation for flat galaxies." Monthly Notices of the Royal Astronomical Society 479, no. 3 (2018): 3373–80. http://dx.doi.org/10.1093/mnras/sty1629.

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20

Courteau, Stephane, and Hans‐Walter Rix. "Maximal Disks and the Tully‐Fisher Relation." Astrophysical Journal 513, no. 2 (1999): 561–71. http://dx.doi.org/10.1086/306872.

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21

Courteau, Stephane, David R. Andersen, Matthew A. Bershady, Lauren A. MacArthur, and Hans‐Walter Rix. "The Tully‐Fisher Relation of Barred Galaxies." Astrophysical Journal 594, no. 1 (2003): 208–24. http://dx.doi.org/10.1086/376754.

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22

Bedregal, A. G., A. Aragón-Salamanca, and M. R. Merrifield. "The Tully–Fisher relation for S0 galaxies." Monthly Notices of the Royal Astronomical Society 373, no. 3 (2006): 1125–40. http://dx.doi.org/10.1111/j.1365-2966.2006.11031.x.

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23

Bureau, M., M. J. Williams, and M. Cappellari. "Lenticular vs spiral galaxies: dark matter content and the Tully-Fisher relation." Proceedings of the International Astronomical Union 5, H15 (2009): 82. http://dx.doi.org/10.1017/s1743921310008355.

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Анотація:

We provide observational constraints on disk galaxy evolution for a sample of 28 local edge-on early-type (S0–Sb) disk galaxies. We do this in two ways: (i) we use simple dynamical modelling techniques to constrain their stellar and dark matter content (Williams et al. 2009) and (ii) we compare the zero points of the Tully-Fisher relations (TFRs; Tully & Fisher 1977) of the spirals and S0s.

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24

Karachentsev, Igor D., Elena I. Kaisina, and Olga G. Kashibadze (Nasonova). "THE LOCAL TULLY–FISHER RELATION FOR DWARF GALAXIES." Astronomical Journal 153, no. 1 (2016): 6. http://dx.doi.org/10.3847/1538-3881/153/1/6.

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25

Freedman, Wendy L. "Local calibrators for the infrared Tully-Fisher relation." Astrophysical Journal 355 (June 1990): L35. http://dx.doi.org/10.1086/185732.

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26

Sorce, Jenny G., Hélène M. Courtois, R. Brent Tully, et al. "CALIBRATION OF THE MID-INFRARED TULLY-FISHER RELATION." Astrophysical Journal 765, no. 2 (2013): 94. http://dx.doi.org/10.1088/0004-637x/765/2/94.

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27

Gurovich, Sebastián, Kenneth Freeman, Helmut Jerjen, Lister Staveley-Smith, and Ivânio Puerari. "THE SLOPE OF THE BARYONIC TULLY-FISHER RELATION." Astronomical Journal 140, no. 3 (2010): 663–76. http://dx.doi.org/10.1088/0004-6256/140/3/663.

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28

Koda, Jin, Yoshiaki Sofue, and Keiichi Wada. "On the Origin of the Tully‐Fisher Relation." Astrophysical Journal 532, no. 1 (2000): 214–20. http://dx.doi.org/10.1086/308579.

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29

Tiley, Alfred L., Martin Bureau, Amélie Saintonge, Selcuk Topal, Timothy A. Davis, and Kazufumi Torii. "The Tully–Fisher relation of COLD GASS Galaxies." Monthly Notices of the Royal Astronomical Society 461, no. 4 (2016): 3494–515. http://dx.doi.org/10.1093/mnras/stw1545.

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30

Dickey, John M., and Ilya Kazes. "The Tully-Fisher relation for the CO line." Astrophysical Journal 393 (July 1992): 530. http://dx.doi.org/10.1086/171526.

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31

Amram, Philippe, Claudia Mendes De Oliveira, Henri Plana, and Chantal Balkowski. "The Tully-Fisher Relation for Hickson Compact Groups." Symposium - International Astronomical Union 220 (2004): 413–14. http://dx.doi.org/10.1017/s0074180900183743.

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Анотація:

We investigate the properties of the B-band Tully-Fisher (TF) relation for 25 compact group galaxies, using Vmax derived from 2-D velocity maps. Our main result is that the majority of the Hickson Compact Group (HCG) galaxies lie on the TF relation, although with large scatter. However, 20% of the galaxies, including the lowest-mass systems, seem to have higher B luminosities, for a given mass, or alternatively, a mass which is too low for their luminosities. We favour the scenario of brightening of the outliers due to either enhanced star formation or merging, rather than truncation of the dark halo due to interactions, to explain the position of the outliers on the TF relation.

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32

Steinmetz, Matthias, and Julio F. Navarro. "The Cosmological Origin of the Tully‐Fisher Relation." Astrophysical Journal 513, no. 2 (1999): 555–60. http://dx.doi.org/10.1086/306904.

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33

Dutton, Aaron A. "The baryonic Tully-Fisher relation and galactic outflows." Monthly Notices of the Royal Astronomical Society 424, no. 4 (2012): 3123–28. http://dx.doi.org/10.1111/j.1365-2966.2012.21469.x.

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34

Bamford, S. P., B. Milvang-Jensen, A. Aragón-Salamanca, and L. Simard. "The Tully—Fisher relation of distant cluster galaxies." Monthly Notices of the Royal Astronomical Society 361, no. 1 (2005): 109–27. http://dx.doi.org/10.1111/j.1365-2966.2005.09135.x.

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35

Bamford, S. P., A. Aragon-Salamanca, and B. Milvang-Jensen. "The Tully-Fisher relation of distant field galaxies." Monthly Notices of the Royal Astronomical Society 366, no. 1 (2006): 308–20. http://dx.doi.org/10.1111/j.1365-2966.2005.09867.x.

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36

Kurbatov, E. P., A. V. Tutukov, and B. M. Shustov. "Evolution of galaxies and the Tully-Fisher relation." Astronomy Reports 49, no. 7 (2005): 510–19. http://dx.doi.org/10.1134/1.1985948.

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37

Sofue, Y., Y. Tutui, M. Honma, et al. "CO Tully-Fisher Relation for the Distance Measurement to Redshift cz=20,000 to 50,000 km/s." Symposium - International Astronomical Union 183 (1999): 70. http://dx.doi.org/10.1017/s0074180900132152.

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The accuracy of measurement of the Hubble constant depends not only on the accuracy of distance measurement but also on how small is the effect of local flows: The larger are redshifts of used galaxies, the higher is the accuracy of H0, if the error in distance measurement is comparable. The HI Tully-Fisher relation has been the standard tool for distance measurement up to cz ∼ 10,000 km s–1 (Tully and Fisher 1977), where, however, the local flow is not negligible.

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38

Rhee, Myung-Hyun, and Adrick H. Broeils. "HI LINEWIDTHS, ROTATION VELOCITIES AND THE TULLY-FISHER RELATION." Journal of Astronomy and Space Sciences 22, no. 2 (2005): 89–112. http://dx.doi.org/10.5140/jass.2005.22.2.089.

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39

Lelli, Federico, Stacy S. McGaugh, and James M. Schombert. "THE SMALL SCATTER OF THE BARYONIC TULLY–FISHER RELATION." Astrophysical Journal 816, no. 1 (2015): L14. http://dx.doi.org/10.3847/2041-8205/816/1/l14.

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40

De Rossi, M. E., P. B. Tissera, and S. E. Pedrosa. "Impact of supernova feedback on the Tully-Fisher relation." Astronomy and Astrophysics 519 (September 2010): A89. http://dx.doi.org/10.1051/0004-6361/201014058.

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41

RHEE, MYUNG-HYUN. "ON THE PHYSICAL BASIS OF THE TULLY-FISHER RELATION." Journal of The Korean Astronomical Society 37, no. 1 (2004): 15–39. http://dx.doi.org/10.5303/jkas.2004.37.1.015.

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42

RHEE, MYUNG-HYUN. "MASS-TO-LIGHT RATIO AND THE TULLY-FISHER RELATION." Journal of The Korean Astronomical Society 37, no. 3 (2004): 91–117. http://dx.doi.org/10.5303/jkas.2004.37.3.091.

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43

van Driel, W., A. C. van den Broek, and W. Baan. "The Tully-Fisher relation of the IRAS minisurvey galaxies." Astrophysical Journal 444 (May 1995): 80. http://dx.doi.org/10.1086/175584.

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44

van Starkenburg, L., P. P. van der Werf, L. Yan, and A. F. M. Moorwood. "On measuring the Tully-Fisher relation atz > 1." Astronomy & Astrophysics 450, no. 1 (2006): 25–37. http://dx.doi.org/10.1051/0004-6361:20053733.

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45

Glowacki, M., E. Elson, and R. Davé. "The baryonic Tully–Fisher relation in the simba simulation." Monthly Notices of the Royal Astronomical Society 498, no. 3 (2020): 3687–702. http://dx.doi.org/10.1093/mnras/staa2616.

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ABSTRACT We investigate the Baryonic Tully–Fisher relation (BTFR) in the $(100\, h^{-1}{\rm Mpc})^3$simba hydrodynamical galaxy formation simulation together with a higher resolution $(25\, h^{-1}{\rm Mpc})^3$simba run, for over 10 000 disc-dominated, H i-rich galaxies. We generate simulated galaxy rotation curves from the mass distribution, which we show yields similar results to using the gas rotational velocities. From this, we measure the galaxy rotation velocity Vcirc using four metrics: $V_{\rm max}, V_{\rm flat}, V_{2R_e},$ and Vpolyex. We compare the predicted BTFR to the SPARC observational sample and find broad agreement. In detail, however, simba is biased towards higher Vcirc by up to 0.1 dex. We find evidence for the flattening of the BTFR in Vcirc &gt; 300 km s−1 galaxies, in agreement with recent observational findings. simba’s rotation curves are more peaked for lower mass galaxies, in contrast with observations, suggesting overly bulge-dominated dwarf galaxies in our sample. We investigate for residuals around the BTFR versus H i mass, stellar mass, gas fraction, and specific star formation rate, which provide testable predictions for upcoming BTFR surveys. simba’s BTFR shows sub-optimal resolution mass convergence, with the higher resolution run lowering V in better agreement with data.

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46

Tonini, Chiara, Claudia Maraston, Bodo Ziegler, et al. "The hierarchical build-up of the Tully-Fisher relation." Monthly Notices of the Royal Astronomical Society 415, no. 1 (2011): 811–28. http://dx.doi.org/10.1111/j.1365-2966.2011.18767.x.

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47

Noordermeer, E., and M. A. W. Verheijen. "The high-mass end of the Tully-Fisher relation." Monthly Notices of the Royal Astronomical Society 381, no. 4 (2007): 1463–72. http://dx.doi.org/10.1111/j.1365-2966.2007.12369.x.

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48

Neill, J. D., Mark Seibert, R. Brent Tully, et al. "THE CALIBRATION OF THEWISEW1 AND W2 TULLY-FISHER RELATION." Astrophysical Journal 792, no. 2 (2014): 129. http://dx.doi.org/10.1088/0004-637x/792/2/129.

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49

Aragón-Salamanca, Alfonso. "The Tully-Fisher relation: evolution with redshift and environment." Proceedings of the International Astronomical Union 2, S235 (2006): 8–11. http://dx.doi.org/10.1017/s1743921306004947.

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Анотація:

AbstractThe Tully-Fisher Relation (TFR) links two fundamental properties of disk galaxies: their luminosity and their rotation velocity (mass). The pioneering work of Vogt et al. in the 1990's showed that it is possible to study the TFR for spiral galaxies at considerable look-back-times, and use it as a powerful probe of their evolution. In recent years, several groups have studied the TFR for galaxies in different environments reaching redshifts beyond one. In this brief review I summarise the main results of some of these studies and their consequences for our understanding of the formation and evolution of disk galaxies. Particular emphasis is placed on the possible environment-driven differences in the behaviour of the TFR for field and cluster galaxies.

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50

Kannappan, Sheila J., Daniel G. Fabricant, and Marijn Franx. "Physical Sources of Scatter in the Tully-Fisher Relation." Astronomical Journal 123, no. 5 (2002): 2358–86. http://dx.doi.org/10.1086/339972.

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