CID-42

Last updated
CID-42
Cid-42.jpg
Optical and X-ray images of CID-42
Observation data (J2000 epoch)
Constellation Sextans
Right ascension 10h 00m 43.13s
Declination +02° 06 37.40
Redshift 0.359 [1]
Heliocentric radial velocity 89302 km/s [2]
Distance 3.9 billion [3]
Apparent magnitude  (V)?
Characteristics
Type Spiral
Mass 4.5x1011 [1]   M
Number of stars?
Apparent size  (V)?
Other designations
CXOC J100043.1+020637 2XMM J100043.1+020637

CID-42 (also known as CXOC J100043.1+020637 [4] ) is a galaxy quasar about 3.9 billion light years away in the constellation Sextans. It is believed to have a supermassive black hole at its center.

Contents

Description

CID-42 is thought to be the result of a galaxy collision between two smaller galaxies. It has a distinctive trail of stars extending many light years. [3]

Black hole

The discovery of a potential black hole was made after combining through the data and images taken by several telescopes including NASA's Chandra X-ray Observatory, the Hubble Space Telescope, the Canada-France-Hawaii Telescope and from the ground-based Magellan and Very Large Telescopes in Chile. [5]

When the two galaxies collided the black holes in their centers collided, forming a single supermassive black hole. The black hole then recoiled from the gravitational waves produced by the merger and is being ejected out of the galaxy at several million miles per hour (~2000 km s−1). [1] [6]

Once ejected it is expected to shine as a displaced quasar for 10 million to 10 billion years until it exhausts its fuel and is no longer recognizable as a quasar. [7]

JWST NIRCam observations were able to rule out the gravitational wave producing recoiling black hole sencario. Instead CID-42 is a merging galaxy with only one active galactic nucleus. [8]

Related Research Articles

<span class="mw-page-title-main">Quasar</span> Active galactic nucleus containing a supermassive black hole

A quasar is an extremely luminous active galactic nucleus (AGN). It is sometimes known as a quasi-stellar object, abbreviated QSO. The emission from an AGN is powered by a supermassive black hole with a mass ranging from millions to tens of billions of solar masses, surrounded by a gaseous accretion disc. Gas in the disc falling towards the black hole heats up and releases energy in the form of electromagnetic radiation. The radiant energy of quasars is enormous; the most powerful quasars have luminosities thousands of times greater than that of a galaxy such as the Milky Way. Quasars are usually categorized as a subclass of the more general category of AGN. The redshifts of quasars are of cosmological origin.

<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">Supermassive black hole</span> Largest type of black hole

A supermassive black hole is the largest type of black hole, with its mass being on the order of hundreds of thousands, or millions to billions, of times the mass of the Sun (M). Black holes are a class of astronomical objects that have undergone gravitational collapse, leaving behind spheroidal regions of space from which nothing can escape, including light. Observational evidence indicates that almost every large galaxy has a supermassive black hole at its center. For example, the Milky Way galaxy has a supermassive black hole at its center, corresponding to the radio source Sagittarius A*. Accretion of interstellar gas onto supermassive black holes is the process responsible for powering active galactic nuclei (AGNs) and quasars.

<span class="mw-page-title-main">Stellar black hole</span> Black hole formed by a collapsed star

A stellar black hole is a black hole formed by the gravitational collapse of a star. They have masses ranging from about 5 to several tens of solar masses. They are the remnants of supernova explosions, which may be observed as a type of gamma ray burst. These black holes are also referred to as collapsars.

<span class="mw-page-title-main">Mass deficit</span>

A mass deficit is the amount of mass that has been removed from the center of a galaxy, presumably by the action of a binary supermassive black hole.

<span class="mw-page-title-main">HE0450-2958</span> Galaxy in the constellation Caelum

HE0450-2958 is an unusual quasar. It has been called the "naked quasar" and the "quasar without a home" because it appears to lack a host galaxy. It is estimated to lie approximately one billion parsecs away.

<span class="mw-page-title-main">Gravitational wave background</span> Random background of gravitational waves permeating the Universe

The gravitational wave background is a random background of gravitational waves permeating the Universe, which is detectable by gravitational-wave experiments, like pulsar timing arrays. The signal may be intrinsically random, like from stochastic processes in the early Universe, or may be produced by an incoherent superposition of a large number of weak independent unresolved gravitational-wave sources, like supermassive black-hole binaries. Detecting the gravitational wave background can provide information that is inaccessible by any other means about astrophysical source population, like hypothetical ancient supermassive black-hole binaries, and early Universe processes, like hypothetical primordial inflation and cosmic strings.

<span class="mw-page-title-main">APM 08279+5255</span> Quasar

APM 08279+5255 is a very distant, broad absorption line quasar located in the constellation Lynx. It is magnified and split into multiple images by the gravitational lensing effect of a foreground galaxy through which its light passes. It appears to be a giant elliptical galaxy with a supermassive black hole and associated accretion disk. It possesses large regions of hot dust and molecular gas, as well as regions with starburst activity.

The Andromeda–Milky Way collision is a galactic collision predicted to occur in about 4.5 billion years between the two largest galaxies in the Local Group—the Milky Way and the Andromeda Galaxy. The stars involved are sufficiently far apart that it is improbable that any of them will individually collide, though some stars will be ejected.

<span class="mw-page-title-main">Hanny's Voorwerp</span> Astronomical object appearing as a bright blob, discovered by Hanny van Arkel

Hanny's Voorwerp is a type of astronomical object called a quasar ionization echo. It was discovered in 2007 by Dutch schoolteacher Hanny van Arkel while she was participating as a volunteer in the Galaxy Zoo project, part of the Zooniverse group of citizen science websites. Photographically, it appears as a bright blob close to spiral galaxy IC 2497 in the constellation Leo Minor.

The Cloverleaf quasar is a bright, gravitationally lensed quasar.

A hypercompact stellar system (HCSS) is a dense cluster of stars around a supermassive black hole that has been ejected from the center of its host galaxy. Stars that are close to the black hole at the time of the ejection will remain bound to the black hole after it leaves the galaxy, forming the HCSS.

<span class="mw-page-title-main">SDSS J0927+2943</span> Unusual quasar

SDSS J0927+2943 is an unusual quasar. It exhibits two sets of optical emission lines with different redshifts. The origin of the two emission line systems is believed to be a gravitational wave recoil event: the ejection of a supermassive black hole from the center of the host galaxy. In this interpretation, one of the emission line systems originates in gas that is bound to the black hole, while the other set is associated with gas that remains in the galaxy.

<span class="mw-page-title-main">RX J1131-1231</span> Supermassive-black-hole-containing quasar in the constellation Crater

RX J1131-1231 is a distant, supermassive-black-hole-containing quasar located about 6 billion light years from Earth in the constellation Crater.

<span class="mw-page-title-main">NGC 1395</span> Galaxy in the constellation Eridanus

NGC 1395 is an elliptical galaxy located in the constellation Eridanus. It is located at a distance of circa 75 million light years from Earth, which, given its apparent dimensions, means that NGC 1395 is about 130,000 light years across. It was discovered by William Herschel on November 17, 1784. It is a member of the Eridanus Cluster.

<span class="mw-page-title-main">Direct collapse black hole</span> High-mass black hole seeds

Direct collapse black holes (DCBHs) are high-mass black hole seeds that form from the direct collapse of a large amount of material. They putatively formed within the redshift range z=15–30, when the Universe was about 100–250 million years old. Unlike seeds formed from the first population of stars (also known as Population III stars), direct collapse black hole seeds are formed by a direct, general relativistic instability. They are very massive, with a typical mass at formation of ~105 M. This category of black hole seeds was originally proposed theoretically to alleviate the challenge in building supermassive black holes already at redshift z~7, as numerous observations to date have confirmed.

<span class="mw-page-title-main">UHZ1</span> Background galaxy containing a quasar

UHZ1 is a background galaxy containing a quasar. At a redshift of approximately 10.1, UHZ1 is at a distance of 13.2 billion light-years, seen when our universe was about 3 percent of its current age. This redshift made it the most distant, and therefore earliest known quasar in the observable universe as of 2023. To detect this object, astronomers working at the Chandra X-ray Observatory used the Abell 2744's cluster mass as a gravitational lens in order to magnify distant objects directly behind it. At the time of discovery, it exceeded the distance record of QSO J0313−1806.

References

  1. 1 2 3 Blecha, Laura; Civano, Francesca (October 4, 2012). "Constraints on the Nature of CID-42". Monthly Notices of the Royal Astronomical Society. 428 (2): 1341–1350. arXiv: 1205.6202 . Bibcode:2013MNRAS.428.1341B. doi: 10.1093/mnras/sts114 .
  2. "3XMM J100043.1+020637". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 4 April 2018.
  3. 1 2 "CID-42". Chandra.Harvard.edu. June 4, 2012. Retrieved September 28, 2012.
  4. Civano, F; Elvis, M; Lanzuisi, G; Jahnke, K; Zamorani, G; Blecha, L; Bongiorno, A; Brusa, M; Comastri, A; Hao, H; Leauthaud, A; Loeb, A; Mainieri, V; Piconcelli, E; Salvato, M; Scoville, N; Trump, J; Vignali, C; Aldcroft, T; Bolzonella, M; Bressert, E; Finoguenov, A; Fruscione, A; Koekemoer, A. M; Cappelluti, N; Fiore, F; Giodini, S; Gilli, R; Impey, C. D; et al. (June 9, 2010). "A Runaway Black Hole in COSMOS". The Astrophysical Journal. 717 (1): 209. arXiv: 1003.0020 . Bibcode:2010ApJ...717..209C. doi:10.1088/0004-637X/717/1/209. S2CID   20466072.
  5. "Giant Black Hole Kicked from Home Galaxy". Chandra.Harvard.edu. June 4, 2012. Retrieved September 28, 2012.
  6. "Supermassive black hole ejected from host galaxy". Space.com . June 6, 2012. Retrieved September 28, 2012.
  7. Civano, F; Elvis, M; et al. (April 10, 2012). "Chandra High resolution Observations of CID-42, a candidate recoiling SMBH". Astrophysical Journal. 752 (1): 49. arXiv: 1205.0815 . Bibcode:2012ApJ...752...49C. doi:10.1088/0004-637X/752/1/49. S2CID   118868093.
  8. Li, Junyao; Zhuang, Ming-Yang; Shen, Yue (2023). "JWST Confirms the Nature of CID-42". The Astrophysical Journal. 961 (1): 19. arXiv: 2307.05852 . Bibcode:2024ApJ...961...19L. doi: 10.3847/1538-4357/ad0e0d .