IC 1101

Last updated

IC 1101
IC 1101 in Abell 2029 (hst 06228 03 wfpc2 f702w pc).jpg
June 1995 image of IC 1101 taken by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Virgo
Right ascension 15h 10m 56.1s [1]
Declination +05° 44′ 41″ [1]
Redshift 0.078054±0.000027 [1] [2]
Heliocentric radial velocity 22,419 km/s (13,931 mi/s) [1]
Distance 354.0 ± 24.8  Mpc (1,154.6 ± 80.9 million  ly)h−1
0.67 [1]
Group or cluster Abell 2029
Apparent magnitude  (V)13.22 [1]
Characteristics
Type cD; S0- [1]
Size123.65 to 169.61  kpc (403,300 to 553,200  ly)
(D25 B-band and total K-band isophotes) [3] [4] [lower-alpha 1]
Apparent size  (V)1'.2 × 0'.6 [1]
Other designations
UGC 9752, [1] PGC 54167, [1] A2029-BCG [1]

IC 1101 is a class S0 supergiant (cD) lenticular galaxy at the center of the Abell 2029 galaxy cluster. It has an isophotal diameter at about 123.65 to 169.61 kiloparsecs (400,000 to 550,000 light-years). It possesses a diffuse core which is the largest known core of any galaxy to date, [5] and contains a supermassive black hole, one of the largest discovered. [5] The galaxy is located at 354.0 megaparsecs (1.15 billion light-years) from Earth. The galaxy was discovered on 19 June 1790, by the British astronomer William Herschel. [6]

Contents

Observation history

IC 1101 was catalogued in the Index Catalogue of galaxies in the late 1800s to the early 1900s, which is where the galaxy got its most-used designation. [7] In a 1964 study of galaxies accompanied by radio sources, IC 1101 was listed as being among the diffuse elliptical galaxies chosen for the study. The study noted that IC 1101 had not been considered as a radio source, but radio emissions similar to galaxies with such emissions were detected. [8]

Almost a decade and a half later, in 1978, astronomer Alan Dressler analyzed 12 very rich clusters of galaxies, among them Abell 2029, where IC 1101 is located in. [9] The following year, he released a paper dedicated solely to IC 1101 and its related dynamics and properties, revealing a rising velocity dispersion profile. [10] After this, he would publish a paper overviewing his recent studies on the cluster and the galaxy. [11]

During 1985, a team of astronomers obtained the spectra of the gas inside several galaxy clusters known to be luminous at X-Ray wavelengths, including Abell 2029. [12] Soon after, an investigation into the dynamics of IC 1101 and the galaxies within a few hundred kiloparsecs of it was conducted. [13]

The centers of galaxy clusters are considered to be among the best laboratories for the study of galaxy and cluster evolution, and so during the late 1980s to early 1990s, numerous papers were released, surveying many brightest cluster galaxies. Among them was IC 1101. [14] [15] [16] R-band (red light) luminosity profiles were soon obtained for IC 1101, revealing a very vast halo of light that could be traced out for more than several hundred kiloparsecs from the galaxy's center. [17]

In 2002, an analysis of Chandra X-ray surveys of the cluster was performed. [18] In 2011, a survey of over 430 brightest cluster galaxies was conducted, among them IC 1101. [19]

In 2017, a redshift survey of the cluster was conducted, allowing a list of velocity dispersions to be created. This constrains the dynamics of the cluster. [20] [21] That same year, an analysis of the galaxy's inner regions using Hubble Space Telescope images found a huge yet diffuse galactic core, accompanied with mass estimates of the central supermassive black hole. [5]

During 2019-2020, 170 local galaxy clusters were surveyed for a study of brightest cluster galaxies, their structures and the intracluster light around them. [22]

Characteristics

Morphology

IC 1101 imaged by the Sloan Digital Sky Survey IC 1101.jpg
IC 1101 imaged by the Sloan Digital Sky Survey

The galaxy is classified as a supergiant elliptical (E) to lenticular (S0) [23] and is the brightest galaxy in A2029 (hence its other designation A2029-BCG; BCG meaning brightest cluster galaxy ). [24] [25] The galaxy's morphological type is debated due to it possibly being shaped like a flat disc but only visible from Earth at its broadest dimensions. A morphology of S0- (Hubble stage -2; see Hubble stage for details) has been given by the Third Reference Catalogue of Bright Galaxies (RC3) in 1991. [3]

Components and Structure

Like most large galaxies, IC 1101 is populated by a number of metal-rich stars, some of which are as much as seven billion years older than the Sun, making it appear golden yellow in color. It has a very bright radio source at the center, which is likely associated with an ultramassive black hole in the mass range of 40–100 billion  M☉ measured using core dynamical models, [5] or alternatively at 50-70 billion  M☉ using gas accretion rate and growth modelling, [26] which would make IC 1101's black hole one of the most massive known to date. The estimates of the mass of IC 1101's black hole are near the upper bound of cosmological limits, [26] and is referred to as an "overmassive" black hole. [5]

IC 1101's mass-to-light ratio has been described as being anomalously high. The galaxy also has a unique velocity dispersion profile, which indicates a massive dark matter halo. It accretes roughly 450 solar masses per year. The galaxy lacks nuclear emission in visible light at its center as well as signs of recent star formation. [27] There is also no evidence of dust lanes in the core. [28]

For many years it was suggested that IC 1101 was at the center of a massive cooling flow within the Abell 2029 cluster, [27] but later observations dismissed this. [18]

A 2017 paper suggests that IC 1101 has the largest core size of any galaxy with a core radius of around 4.2 ± 0.1  kpc (13.70 ± 0.33 thousand  ly ) by fitting a model to a Hubble Space Telescope (HST) image of the galaxy. This makes its core larger than the one observed in A2261-BCG, which is 3.2  kpc (10 thousand  ly ). The core is also roughly an order of magnitude larger than the cores of other large elliptical galaxies, such as NGC 4889 and NGC 1600. Estimates of the absolute magnitude of IC 1101's spheroid are very faint for such a large core, indicating a large stellar mass deficit estimated at 4.9×1011 MSun and a large luminosity deficit estimated at 1.1×1011 L☉. A hypothesis for the observed properties and peculiarities of the core is that the merger of the central black holes from the formation of the galaxy flung stars out of the core. [5] However, when examining large and diffuse galactic cores, caution must be taken, as various estimates may differ between the computer models used. As an example, Holmberg 15A was originally claimed to have the largest galactic core of any galaxy but other studies proved otherwise, either not finding a core or estimating a smaller size for it. It should also be noted that the satellite galaxies might have had an effect on the estimated properties of the diffuse core. [28]

IC 1101's major axis is oriented in the northeast to southwest direction. The major axis is even aligned on the axis by which Abell 2029 accretes from Abell 2033. [29] Its components such as the core and main body are well-aligned, but the halo is twisted by 20 degrees from the galaxy's other components. Its isophotes (The shapes connecting areas with the same surface brightness) are predominantly boxy. Closer to the core, IC 1101's isophotes become elongated, suggesting a nuclear disc. This feature might be due to an unresolved double nucleus, produced by a low intensity active galactic nucleus(AGN) or a disrupted satellite galaxy disturbed by the central black hole. Several elliptical galaxies like NGC 4438-B, NGC 5419, VCC 128 contain two point-sources, producing high ellipticities. The NRAO VLA sky-survey detected a radio source near IC 1101, corroborating a possible AGN. Another, weaker radio source has also been detected nearby, opening up the possibility of a double AGN that cannot be ruled out. [28]

Like most BCGs, IC 1101 has a massive and diffuse stellar halo and has some excessive halo light. [30] The halo is twisted by 20 degrees from the main body and core of IC 1101. This feature, among others, seems to be the reason why IC 1101 is classified as a lenticular galaxy In RC3. [28]

IC 1101 imaged by the 9th data release of the Legacy survey. IC 1101 ls-dr9.jpg
IC 1101 imaged by the 9th data release of the Legacy survey.

Size

IC 1101 is considered a large galaxy characterized by an extensive, diffuse halo. This is the intracluster light, or ICL, free-flying stars that are not bound to any galaxy. This ubiquitous mass of stars within galaxy clusters are usually more concentrated around the brightest cluster galaxies, such as IC 1101, however. [31] Photometrically, the ICL is indistinguishable from the brightest cluster galaxy, but it can be distinguished kinematically. [22] During the early 2000s, weak-lensing estimates for Abell 2029 were taken, indicating the distribution of the mass throughout the cluster and galaxy. [32] Defining the size of a galaxy varies according to the method used in the astronomical literature. Photographic plates of blue light from the galaxy (sampling stars excluding the diffuse halo) yield an effective radius (the radius within which half the light is emitted) of 65 ± 12  kpc (212 ± 39 thousand  ly ) [27] based on an earlier distance measurement. The galaxy has a very large halo of much lower intensity "diffuse light" extending to a radius of 600 kpc (2 million ly). [30] [ verification needed ] The authors of the study identifying the halo conclude that IC 1101 is "possibly one of the largest and most luminous galaxies in the universe". This view has been stated in several other papers as well, but this figure was based on an earlier assumed distance of 262 megaparsecs (855 million light-years).

More recent measurements, using the 25.0 magnitude/arcsec2 standard (commonly [2] [26] known as D25, a method recommended by R.O. Redman in 1936) [33] [lower-alpha 2] has been utilized by the RC3 in the B-band, with a measured major axis (log 2a+1) of 1.08 (equivalent to 72.10 arcseconds), [3] translating to a diameter of 123.65 kiloparsecs (403,000 ly). [1] Another calculation by the Two Micron All-Sky Survey using the "total" aperture at the K-band yields a much larger size of 169.61 kiloparsecs (553,000 ly). [4] Both measurements are based on the currently-accepted distance to IC 1101. This would make it one of the largest and most luminous galaxies known, though there are other galaxies with larger isophotal diameter measurements (such as NGC 623, Abell 1413 BCG, and ESO 306-17).

Distance

The distance to IC 1101 has also been uncertain, with different methods across different wavelengths producing varying results. An earlier distance calculation from 1980 using the galaxy's photometric property yield a distance of 262.0 Mpc (855 million ly) and a redshift of z = 0.077, based on a Hubble constant value H0 of 60 km/s/Mpc. [34] The RC3 catalogue gave a nearly similar value of z=0.078, based on optical emission lines, [3] a value conformed to as recently as 2017 based on luminosity, stellar mass, and velocity dispersion functions, [2] all yielding distances of 354.0 megaparsecs (1.2 billion light-years) based on the modern value of the Hubble constant H0 = 67.8 km/s/Mpc; the currently accepted values. Lower redshifts have been calculated for other wavelengths such as the photometric redshift measurement by the Two Micron All-Sky Survey (2MASS) in 2014, which gave a value of z = 0.045, [35] translating to a distance of 197.1 megaparsecs (643 million light-years). A measurement made in 2005 by the Arecibo Observatory using the 21-cm hydrogen emission line yields a redshift of z = 0.021, [36] and hence a distance of 97.67 ± 6.84 megaparsecs (318.6 ± 22.3 million light-years).

Formation

The lack of other bright and luminous galaxies other than IC 1101 at the center of the Abell 2029 galaxy cluster suggests that they were absorbed and consumed ("chewed-up") by the nascent IC 1101. Since the halo is somewhat flattened, the halo most likely retained the distribution of the bright luminous galaxies as they were consumed. [10]

The depleted core and other characteristics of IC 1101 such as the halo component and its structure at moderate distances from the center suggest that the galaxy underwent numerous galactic mergers and interactions, perhaps as much as 10, or even more. [5] The smoothness of the halo suggests that it formed early in the history of the cluster. [25] [10] [28]

See also

Notes

  1. ↑ The diameters given at NED were based on a redshift-independent distance measurement. The diameters given here were based on NED's provided scale "Virgo + GA + Shapley" multiplied with the given angular diameter values of the estimation methods being stated.
  2. ↑ Date mistakenly stated as 1963.

Related Research Articles

<span class="mw-page-title-main">Virgo Supercluster</span> Galactic supercluster containing the Virgo Cluster

The Virgo Supercluster or the Local Supercluster is a mass concentration of galaxies containing the Virgo Cluster and Local Group, which itself contains the Milky Way and Andromeda galaxies, as well as others. At least 100 galaxy groups and clusters are located within its diameter of 33 megaparsecs. The Virgo SC is one of about 10 million superclusters in the observable universe and is in the Pisces–Cetus Supercluster Complex, a galaxy filament.

<span class="mw-page-title-main">Messier 87</span> Elliptical galaxy in the Virgo Galaxy Cluster

Messier 87 is a supergiant elliptical galaxy in the constellation Virgo that contains several trillion stars. One of the largest and most massive galaxies in the local universe, it has a large population of globular clusters—about 15,000 compared with the 150–200 orbiting the Milky Way—and a jet of energetic plasma that originates at the core and extends at least 1,500 parsecs, traveling at a relativistic speed. It is one of the brightest radio sources in the sky and a popular target for both amateur and professional astronomers.

<span class="mw-page-title-main">Abell 2218</span> Galaxy cluster in the constellation Draco

Abell 2218 is a large cluster of galaxies over 2 billion light-years away in the constellation Draco.

<span class="mw-page-title-main">Abell 2029</span> Large galaxy cluster in the constellation Virgo

Abell 2029 or A2029 is a large and relaxed cluster of galaxies 315 megaparsecs away in the constellation Virgo. A2029 is a Bautz–Morgan classification type I cluster due to its large central galaxy, IC 1101. Abell 2029 has a diameter of 5.8–8 million light-years. This type of galaxy is called a cD-type brightest cluster galaxy and may have grown to its large size by accreting nearby galaxies. Despite its relaxed state, it is the central member of a large supercluster which shows clear signs of interaction.

<span class="mw-page-title-main">Type-cD galaxy</span> Galaxy morphology classification

The type-cD galaxy is a galaxy morphology classification, a subtype of type-D giant elliptical galaxy. Characterized by a large halo of stars, they can be found near the centres of some rich galaxy clusters. They are also known as supergiant ellipticals or central dominant galaxies.

<span class="mw-page-title-main">Abell 1413</span> Galaxy cluster in constellation Coma Berenices

Abell 1413 is a massive and rich type I galaxy cluster straddling the border between the constellations Leo and Coma Berenices, with the projected comoving distance of approximately 640 Mpc (2.1 billion ly). The cluster is especially notable due to the presence of its very large brightest cluster galaxy (BCG), one of the most extreme examples of its type, as well as one of the largest galaxies known. The cluster was first noted by George O. Abell in 1958.

<span class="mw-page-title-main">Abell 665</span> Galaxy cluster in the constellation Ursa Major

Abell 665 is a galaxy cluster in the Abell catalogue in the constellation Ursa Major. It is also known as the only cluster in his 1989 catalog to receive Abell's highest richness class of 5. This means that it contains at least 300 galaxies in the magnitude range of m3 to m3+2, where m3 is the magnitude of the third-brightest member of the cluster. The clusters in all other richness classes contain less than 300 such galaxies. Abell 665's combination of high brightness and large distance, made it an excellent candidate along with 37 other clusters to help determine the Hubble constant using the Sunyaev–Zel'dovich effect in 2006.

<span class="mw-page-title-main">NGC 6166</span> Galaxy in the constellation Hercules

NGC 6166 is an elliptical galaxy in the Abell 2199 cluster. It lies 490 million light years away in the constellation Hercules. The primary galaxy in the cluster, it is one of the most luminous galaxies known in terms of X-ray emissions.

<span class="mw-page-title-main">Holmberg 15A</span> Elliptical galaxy in the constellation Cetus

Holmberg 15A is a supergiant elliptical galaxy and the central dominant galaxy of the Abell 85 galaxy cluster in the constellation Cetus, about 700 million light-years from Earth. It was discovered c. 1937 by Erik Holmberg. It became well known when it was reported to have the largest core ever observed in a galaxy, spanning some 15,000 light years, however this was subsequently refuted.

Abell 2152 is a bimodal galaxy cluster and one of three clusters comprising the Hercules Supercluster. It contains 3 BCGs; the S0 lenticular UGC 10204, the pair UGC 10187, and the SA0 unbarred lenticular CGCG 108-083. In total there are 41 galaxies which are confirmed to be members of the cluster. The cluster is classified as a Bautz-Morgan type III and Rood-Sastry class F cluster, indicating morphological irregularity and perhaps dynamical youth. It is receding from the Milky Way galaxy with a velocity of 12385 km/s.

<span class="mw-page-title-main">Abell 1201 BCG</span> Galaxy in the constellation Leo

Abell 1201 BCG (short for Abell 1201 Brightest Cluster Galaxy) is a type-cD massive elliptical galaxy residing as the brightest cluster galaxy (BCG) of the Abell 1201 galaxy cluster. At a redshift of 0.169, this system is around 2.7 billion light-years from Earth, and offset about 11 kiloparsecs from the X-ray peak of the intracluster gas. With an ellipticity of 0.32±0.02, the stellar distribution is far from spherical. In solar units, the total stellar luminosity is 4×1011 L☉ in SDSS r-band, and 1.6×1012 L☉ in 2MASS K-band. Half the stars orbit within an effective radius of 15 kpc, and their central velocity dispersion is about 285 km s−1 within 5 kpc rising to 360 km s−1 at 20 kpc distance.

<span class="mw-page-title-main">ESO 444-46</span> Galaxy in the constellation Centaurus

ESO 444-46 is a class E4 supergiant elliptical galaxy; the dominant and brightest member of the Abell 3558 galaxy cluster around 640 million light-years away in the constellation Centaurus. It lies within the core of the massive Shapley Supercluster, one of the closest neighboring superclusters. It is one of the largest galaxies in the local universe, and possibly contains one of the most massive black holes known. The black hole's mass is very uncertain, with estimates ranging from as low as 501 million M☉, to as high as 77.6 billion M☉.

<span class="mw-page-title-main">NGC 3311</span> Galaxy in the constellation Hydra

NGC 3311 is a super-giant elliptical galaxy located about 190 million light-years away in the constellation Hydra. The galaxy was discovered by astronomer John Herschel on March 30, 1835. NGC 3311 is the brightest member of the Hydra Cluster and forms a pair with NGC 3309 which along with NGC 3311, dominate the central region of the Hydra Cluster.

<span class="mw-page-title-main">NGC 708</span> Galaxy in the constellation Andromeda

NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 Seyfert galaxy.

Abell 1146 is a rich galaxy cluster in the constellation Crater. Its richness class is 4, and it is located about 2 billion light-years away.

<span class="mw-page-title-main">IC 1459</span> Elliptical galaxy in the constellation of Grus

IC 1459 is an elliptical galaxy located in the constellation Grus. It is located at a distance of circa 85 million light-years from Earth, which, given its apparent dimensions, means that IC 1459 is about 130,000 light-years across. It was discovered by Edward Emerson Barnard in 1892.

<span class="mw-page-title-main">ESO 383-76</span> Elliptical galaxy in the constellation Centaurus

ESO 383-76 is an elongated, X-ray luminous supergiant elliptical galaxy, residing as the dominant, brightest cluster galaxy (BCG) of the Abell 3571 galaxy cluster, the sixth-brightest in the sky at X-ray wavelengths. It is located at the distance of 200.6 megaparsecs from Earth, and is possibly a member of the large Shapley Supercluster. With a diameter of about 540.89 kiloparsecs, it is one of the largest galaxies known.

References

  1. 1 2 3 4 5 6 7 8 9 10 11 12 "NED results for object IC 1101". NASA/IPAC Extragalactic Database. Retrieved 28 August 2022.
  2. 1 2 3 "Reference Lookup | NASA/IPAC Extragalactic Database". ned.ipac.caltech.edu. Retrieved 9 December 2022.
  3. 1 2 3 4 De Vaucouleurs, Gerard; De Vaucouleurs, Antoinette; Corwin, Herold G.; Buta, Ronald J.; Paturel, Georges; Fouque, Pascal (1991). Third Reference Catalogue of Bright Galaxies. Bibcode:1991rc3..book.....D.
  4. 1 2 "NASA/IPAC Extragalactic Database". Archived from the original on 15 August 2022. Retrieved 26 August 2022.
  5. 1 2 3 4 5 6 7 Dullo, Bililign T.; Graham, Alister W.; Knapen, Johan H. (October 2017). "A remarkably large depleted core in the Abell 2029 BCG IC 1101". Monthly Notices of the Royal Astronomical Society. 471 (2): 2321–2333. arXiv: 1707.02277 . Bibcode:2017MNRAS.471.2321D. doi:10.1093/mnras/stx1635. S2CID   119000593.
  6. ↑ "William Herschel's astronomical discoveries". MacTutor. University of St Andrews, Scotland. Retrieved 4 April 2020.
  7. ↑ Dreyer, J. L. E. (1895). "Index Catalogue of Nebulae found in the years 1888 to 1894, with Notes and Corrections to the New General Catalogue". Memoirs of the Royal Astronomical Society . 51: 185–228. Bibcode:1895MmRAS..51..185D.
  8. ↑ Matthews, Thomas A.; Morgan, William W.; Schmidt, Maarten (July 1964). "A Discussion of Galaxies Identified with Radio Sources". Astrophysical Journal. 140: 32,35. Bibcode:1964ApJ...140...35M. doi:10.1086/147890 . Retrieved 21 April 2023.
  9. ↑ Dressler, A. (August 1978). "A comprehensive study of 12 very rich clusters of galaxies. I. Photometric technique and analysis of the luminosity function". Astrophysical Journal. 223: 15. Bibcode:1978ApJ...223..765D. doi: 10.1086/156310 .
  10. 1 2 3 Dressler, A. (August 1979). "The dynamics and structure of the cD galaxy in Abell 2029". Astrophysical Journal. 231: 659–670. Bibcode:1979ApJ...231..659D. doi:10.1086/157229 . Retrieved 17 January 2023.
  11. ↑ Dressler, A. (1981). "The dynamics of the cluster of galaxies A 2029". Astrophysical Journal. 243: 6. Bibcode:1981ApJ...243...26D. doi:10.1086/158562 . Retrieved 27 February 2022.
  12. ↑ Hu, E.M.; Cowie, L.L.; Wang, Z. (December 1985). "Long-slit spectroscopy of gas in the cores of X-ray luminous clusters". Astrophysical Journal Supplement Series. 59: 53. Bibcode:1985ApJS...59..447H. doi:10.1086/191081.
  13. ↑ Bower, R.G.; Ellis, R.S.; Efstathiou, G. (October 1988). "A study of satellite galaxies in the rich cluster A 2029.p". Monthly Notices of the Royal Astronomical Society. 234 (3): 725. Bibcode:1988MNRAS.234..725B. doi:10.1093/mnras/234.3.725 . Retrieved 24 February 2023.
  14. ↑ Schombert, James M. (March 1986). "The Structure of Brightest Cluster Members. I. Surface Photometry". Astrophysical Journal. 60: 91. Bibcode:1986ApJS...60..603S. doi: 10.1086/191100 .
  15. ↑ Schombert, James M. (August 1987). "The Structure of Brightest Cluster Members. II. Mergers". Astrophysical Journal Supplement. 64: 24. Bibcode:1987ApJS...64..643S. doi:10.1086/191212 . Retrieved 3 March 2023.
  16. ↑ Schombert, James M. (1988). "The Structure of Brightest Cluster Members. III. cD Envelopes". Astrophysical Journal. 328: 14. Bibcode:1988ApJ...328..475S. doi:10.1086/166306 . Retrieved 3 March 2023.
  17. ↑ Boughn, S.P.; Kuhn, J.R.; Uson, Juan M. (1990). "CCD Observation of Diffuse Light in the Rich Cluster A:2029". The Galactic and Extragalactic Background Radiation. 139: 7. Bibcode:1990IAUS..139..357B . Retrieved 12 March 2023.
  18. 1 2 Lewis, Aaron D.; Stocke, John T.; Buote, David A. (July 2002). "Chandra Observations of Abell 2029: No Cooling Flow and a Steep Abundance Gradient". The Astrophysical Journal. 573 (1): 5. arXiv: astro-ph/0205374 . Bibcode:2002ApJ...573L..13L. doi:10.1086/341990. S2CID   18050535 . Retrieved 27 February 2023.
  19. ↑ Donzelli, C.G.; Muriel, H.; Madrid, J.P. (August 2011). "The Luminosity Profiles of Brightest Cluster Galaxies". The Astrophysical Journal Supplement. 195 (2): 15. arXiv: 1109.0996 . Bibcode:2011ApJS..195...15D. doi:10.1088/0067-0049/195/2/15. S2CID   119306897 . Retrieved 27 February 2023.
  20. ↑ Sohn, Jubee; Geller, Margaret J.; Zahid, H. Jabran; Fabricant, Daniel G.; Diaferio, Antonaldo; Rines, Kenneth J. (April 2017). "The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma". The Astrophysical Journal. 229 (2): 16. arXiv: 1612.06428 . Bibcode:2017ApJS..229...20S. doi: 10.3847/1538-4365/aa653e . S2CID   55210136.
  21. ↑ Sohn, Jubee; Geller, Margaret J.; Walker, Stephen A.; Dell'Antonio, Ian; Diaferio, Antonaldo; Rines, Kenneth J. (January 2019). "The Massively Accreting Cluster A2029". The Astrophysical Journal. 871 (1): 15. arXiv: 1808.00488 . Bibcode:2019ApJ...871..129S. doi: 10.3847/1538-4357/aaf1cc . S2CID   102483413.
  22. 1 2 Kluge, M.; Neureiter, B.; Riffeser, A.; Bender, R.; Gossel, C.; Hopp, U.; Schmidt, M.; Ries, C.; Brosch, N. (April 2020). "Structure of Brightest Cluster Galaxies and Intracluster Light". The Astrophysical Journal. 247 (2): 5194–5199. arXiv: 1908.08544 . Bibcode:2020ApJS..247...43K. doi: 10.3847/1538-4365/ab733b . PMID   43. S2CID   201645169.
  23. ↑ "IC 1101". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 21 December 2014.
  24. ↑ Lewis, Aaron D.; Buote, David A.; Stocke, John T. (March 2003). "Chandra Observations of A2029: The Dark Matter Profile Down to below 0.01rvir in an Unusually Relaxed Cluster". The Astrophysical Journal . 586 (1): 135–142. arXiv: astro-ph/0209205 . Bibcode:2003ApJ...586..135L. doi:10.1086/367556. S2CID   119439086.
  25. 1 2 Uson, Juan M.; Boughn, Stephen P.; Kuhn, Jeffrey R. (October 1990). "The central galaxy in Abell 2029 - an old supergiant". Science . 250 (4980): 539–540. Bibcode:1990Sci...250..539U. doi:10.1126/science.250.4980.539. PMID   17751483. S2CID   23362384.
  26. 1 2 3 Brockamp, M.; Baumgardt, H.; Britzen, S.; Zensus, A. (January 2016). "Unveiling Gargantua: A new search strategy for the most massive central cluster black holes". Astronomy & Astrophysics. 585. A153. arXiv: 1509.04782 . Bibcode:2016A&A...585A.153B. doi:10.1051/0004-6361/201526873. S2CID   54641547.
  27. 1 2 3 Fisher, David; Illingworth, Garth; Franx, Marijn (January 1995). "Kinematics of 13 brightest cluster galaxies". The Astrophysical Journal . 438 (2): 539–562. Bibcode:1995ApJ...438..539F. doi:10.1086/175100.
  28. 1 2 3 4 5 Dullo, Bililign T. (December 2019). "The Most Massive Galaxies with Large Depleted Cores: Structural Parameter Relations and Black Hole Masses". The Astrophysical Journal. 886 (2): 80. arXiv: 1910.10240 . Bibcode:2019ApJ...886...80D. doi: 10.3847/1538-4357/ab4d4f . S2CID   204838306.
  29. ↑ Gonzalez, Elizabeth Johana; de Los Rios, Martin; Oio, Gabriel A.; Hernández Lang, Daniel; Aguirre Tagliferro, Tania; Domínguez R., Mariano J.; Nilo Castellón, José Luis; Cuevas L., Héctor; Valotto, Carlos A. (March 2018). "Analysis of candidates for interacting galaxy clusters. I. A1204 and A2029/A2033". Astronomy & Astrophysics. 611: 12. arXiv: 1801.01498 . Bibcode:2018A&A...611A..78G. doi:10.1051/0004-6361/201732003. S2CID   125690394 . Retrieved 12 February 2023.
  30. 1 2 Uson, Juan M.; Boughn, Stephen P.; Kuhn, Jeffrey R. (March 1991). "Diffuse light in dense clusters of galaxies. I. R-band observations of Abell 2029". The Astrophysical Journal . 369: 46–53. Bibcode:1991ApJ...369...46U. doi:10.1086/169737.
  31. ↑ Montes, Mireia (March 2022). "The faint light in groups and clusters of galaxies". Nature Astronomy. 6 (3): 308–316. arXiv: 2203.06199 . Bibcode:2022NatAs...6..308M. doi:10.1038/s41550-022-01616-z. S2CID   247446707 . Retrieved 12 February 2023.
  32. ↑ Ménard, B.; Erben, T.; Mellier, Y. (2003). "Weak Lensing Study of Abell 2029". Astronomical Society of the Pacific. 301: 5. arXiv: astro-ph/0209190 . Bibcode:2003ASPC..301..537M . Retrieved 12 February 2023.
  33. ↑ "Dimensions of Galaxies". ned.ipac.caltech.edu. Retrieved 9 December 2022.
  34. ↑ Hoessel, J. G.; Gunn, J. E.; Thuan, T. X. (1980). "The photometry properties of brightest cluster galaxies. I. Absolute magnitudes in 116 nearby Abell clusters". The Astrophysical Journal. 241: 486. Bibcode:1980ApJ...241..486H. doi:10.1086/158363.
  35. ↑ Bilicki, Maciej; Jarrett, Thomas H.; Peacock, John A.; Cluver, Michelle E.; Steward, Louise (2014). "Two Micron All Sky Survey Photometric Redshift Catalog: A Comprehensive Three-dimensional Census of the Whole Sky". The Astrophysical Journal Supplement Series. 210 (1): 9. arXiv: 1311.5246 . Bibcode:2014ApJS..210....9B. doi:10.1088/0067-0049/210/1/9. S2CID   118733998.
  36. ↑ Springob, Christopher M.; Haynes, Martha P.; Giovanelli, Riccardo; Kent, Brian R. (2005). "A Digital Archive of H I 21 Centimeter Line Spectra of Optically Targeted Galaxies". The Astrophysical Journal Supplement Series. 160 (1): 149. arXiv: astro-ph/0505025 . Bibcode:2005ApJS..160..149S. doi:10.1086/431550. S2CID   14911447.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.