Share to: share facebook share twitter share wa share telegram print page

 

Cloverleaf quasar

Cloverleaf, H1413+117, QSO 1415+1129
ESO image of the Cloverleaf quasar
Observation data (Epoch J2000)
Right ascension14 h 15 m 46.27 s
Declination+11°  29 ′  43.4 ″
Redshift2.56
Distance11 Gly
Apparent magnitude (V)17
Notable featuresFour-image lens, bright CO emission
Other designations
QSO J1415+1129, QSO B1413+1143, H 1413+117, Clover Leaf Quasar
See also: Quasar, List of quasars

The Cloverleaf quasar (H1413+117, QSO J1415+1129) is a bright, gravitationally lensed quasar. It receives its name because of gravitational lensing spitting the single quasar into four images.[1]

Quasar

Molecular gas (notably CO) detected in the host galaxy associated with the quasar is the oldest molecular material known and provides evidence of large-scale star formation in the early universe. Thanks to the strong magnification provided by the foreground lens, the Cloverleaf is the brightest known source of CO emission at high redshift[2] and was also the first source at a redshift z = 2.56 to be detected with HCN[3] or HCO+ emission.[4] This suggests the quasar is currently undergoing an intense wave of star formations thus increasing its luminosity.[3] A radio jet has also been found on the side of quasar according to a study published in 2023.[5]

CCD image of the Cloverleaf quasar taken in March 1988 by the ESO/MPI 2.2m telescope. The four separated images are part of the quasar.

The 4 quasar images were originally discovered in 1984; in 1988, they were determined to be a single quasar split into four images, instead of 4 separate quasars. The X-rays from iron atoms were also enhanced relative to X-rays at lower energies. Since the amount of brightening due to gravitational lensing doesn't vary with the wavelength, this means that an additional object has magnified the X-rays. The increased magnification of the X-ray light can be explained by gravitational microlensing, an effect which has been used to search for compact stars and planets in our galaxy. Microlensing occurs when a star or a multiple star system passes in front of light from a background object. If a single star or a multiple star system in one of the foreground galaxies passed in front of the light path for the brightest image, then that image would be selectively magnified.[6]

Black hole

The X-rays would be magnified much more than the visible light if they came from a region around the central supermassive black hole of the lensing galaxy that was smaller than the origin region of the visible light. The enhancement of the X-rays from iron ions would be due to this same effect. The analysis indicates that the X-rays are coming from a very small region, about the size of the Solar System, around the central black hole. The visible light is coming from a region ten or more times larger. The angular size of these regions at a distance of 11 billion light years is tens of thousands times smaller than the smallest region that can be resolved by the Hubble Space Telescope. This provides a way to test models for the flow of gas around a supermassive black hole.[6] Additionally, inner regions of the quasar's accretion disk around the black hole has been detected suggesting outflow wind.[7]

Lensing galaxy and partial Einstein ring

Data from NICMOS and a special algorithm resolved the lensing galaxy and a partial Einstein ring. The Einstein ring represents the host galaxy of the lensed quasar.[8]

History

The Cloverleaf quasar was discovered in 1988. Data on the Cloverleaf collected by the Chandra X-ray Observatory in 2004 were compared with that gathered by optical telescopes. One of the X-ray components (A) in the Cloverleaf is brighter than the others in both optical and X-ray light but was found to be relatively brighter in X-ray than in optical light. The X-rays from iron atoms were also enhanced relative to X-rays at lower energies.[6]

See also

References

  1. ^ [email protected]. "The Cloverleaf quasar". www.eso.org. Retrieved 2024-08-28.
  2. ^ S. Venturini; P. M. Solomon (2003). "The Molecular Disk in the Cloverleaf Quasar". Astrophysical Journal. 590 (2): 740–745. arXiv:astro-ph/0210529. Bibcode:2003ApJ...590..740V. doi:10.1086/375050. S2CID 761080.
  3. ^ a b P. Solomon; P. Vanden Bout; C. Carilli; M. Guelin (2003). "The Essential Signature of a Massive Starburst in a Distant Quasar". Nature. 426 (6967): 636–638. arXiv:astro-ph/0312436. Bibcode:2003Natur.426..636S. doi:10.1038/nature02149. PMID 14668856. S2CID 4414417.
  4. ^ D. A. Riechers; et al. (2006). "First Detection of HCO+ Emission at High Redshift". Astrophysical Journal Letters. 645 (1): L13 – L16. arXiv:astro-ph/0605437. Bibcode:2006ApJ...645L..13R. doi:10.1086/505908. S2CID 17504751.
  5. ^ Zhang, Lei; Zhang, Zhi-Yu; Nightingale, James W.; Zou, Ze-Cheng; Cao, Xiaoyue; Tsai, Chao-Wei; Yang, Chentao; Shi, Yong; Wang, Junzhi; Xu, Dandan; Lin, Ling-Rui; Zhou, Jing; Li, Ran (2023-09-01). "Discovery of a radio jet in the Cloverleaf quasar at z = 2.56". Monthly Notices of the Royal Astronomical Society. 524 (3): 3671–3682. arXiv:2212.07027. Bibcode:2023MNRAS.524.3671Z. doi:10.1093/mnras/stad2069. ISSN 0035-8711.
  6. ^ a b c "Chandra :: Photo Album :: Cloverleaf Quasar (a.k.a. H1413+117) :: More Images of the Cloverleaf Quasar". chandra.harvard.edu. Retrieved 2024-08-28.
  7. ^ Chartas, G.; Eracleous, M.; Dai, X.; Agol, E.; Gallagher, S. (2007-06-01). "Discovery of Probable Relativistic Fe Emission and Absorption in the Cloverleaf Quasar H 1413+117". The Astrophysical Journal. 661 (2): 678–692. arXiv:astro-ph/0702742. Bibcode:2007ApJ...661..678C. doi:10.1086/516816. ISSN 0004-637X.
  8. ^ Chantry, Virginie; Magain, Pierre (August 2007). "Deconvolution of HST images of the Cloverleaf gravitational lens : detection of the lensing galaxy and a partial Einstein ring". Astronomy & Astrophysics. 470 (2): 467–473. arXiv:astro-ph/0612094. Bibcode:2007A&A...470..467C. doi:10.1051/0004-6361:20066839. ISSN 0004-6361.

Further reading

Kembali kehalaman sebelumnya


Index: pl ar de en es fr it arz nl ja pt ceb sv uk vi war zh ru af ast az bg zh-min-nan bn be ca cs cy da et el eo eu fa gl ko hi hr id he ka la lv lt hu mk ms min no nn ce uz kk ro simple sk sl sr sh fi ta tt th tg azb tr ur zh-yue hy my ace als am an hyw ban bjn map-bms ba be-tarask bcl bpy bar bs br cv nv eml hif fo fy ga gd gu hak ha hsb io ig ilo ia ie os is jv kn ht ku ckb ky mrj lb lij li lmo mai mg ml zh-classical mr xmf mzn cdo mn nap new ne frr oc mhr or as pa pnb ps pms nds crh qu sa sah sco sq scn si sd szl su sw tl shn te bug vec vo wa wuu yi yo diq bat-smg zu lad kbd ang smn ab roa-rup frp arc gn av ay bh bi bo bxr cbk-zam co za dag ary se pdc dv dsb myv ext fur gv gag inh ki glk gan guw xal haw rw kbp pam csb kw km kv koi kg gom ks gcr lo lbe ltg lez nia ln jbo lg mt mi tw mwl mdf mnw nqo fj nah na nds-nl nrm nov om pi pag pap pfl pcd krc kaa ksh rm rue sm sat sc trv stq nso sn cu so srn kab roa-tara tet tpi to chr tum tk tyv udm ug vep fiu-vro vls wo xh zea ty ak bm ch ny ee ff got iu ik kl mad cr pih ami pwn pnt dz rmy rn sg st tn ss ti din chy ts kcg ve 
Prefix: a b c d e f g h i j k l m n o p q r s t u v w x y z 0 1 2 3 4 5 6 7 8 9