Astronomy:IRAS F17179+5444

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IRAS F17179+5444
SDSS image of IRAS F17179+5444.
Observation data (J2000.0 epoch)
ConstellationDraco
Right ascension 17h 18m 54.38s[1]
Declination+54° 41′ 48.32″[1]
Redshift0.147680[1]
Helio radial velocity44,273 km/s[1]
Distance1.927 Gly
Characteristics
TypeULIRG Sy2[1]
Size~214,900 ly (65.89 kpc) (estimated)[1]
Other designations
2MASX J17185436+5441486, IRAS 17179+5444, LEDA 165729, TXS 1717+547, CORALZ J171854+544148, SDSS J171854.39+544148.4[1]

IRAS F17179+5444 is a Seyfert type 2 galaxy[2] located in the constellation of Draco. The redshift of the object is (z) 0.147[1] and it was first discovered by astronomers in 1994 from the QDOT survey, designated as QDOT 171754.3+544450.[3] It is classified as an ultraluminous infrared galaxy with a star formation rate of 2.29 ± 0.05 Mʘ per year.[4][3][2]

Description

IRAS F17179+5444 is described as a compact galaxy merger. It has a single nucleus, indicating the nuclei have completely coalesced with each other. It is also surrounded by tidal debris with an extension towards the southwest.[5] Hubble Space Telescope continuum imaging shows the morphology of IRAS F17179+5444 to be complex, with two condensation components connected together by a bridge of diffused radio emission in its nuclear region. In the south of the region a long trail of continuum emission is seen emerging towards the southeast of the galaxy's side by 15 kiloparsecs. A series of dust features are seen crossing the nuclear regions of the galaxy.[6]

The galaxy is found to contain a gigahertz-peaked spectrum (GPS) radio source based on Very Long Baseline Interferometry (VLBI) imaging.[2][7] It has two components found having a separation of 68 milliarcseconds when imaged at 1.6 GHz. However, a 5 GHz high-resolution image also showed it has two much weaker components.[8] Observations also found it is a radio-loud object with a power of 1025.23 W Hz-1 and a low frequency turnover.[9][10]

IRAS F17179+5444 has warm ionized outflows. Based on studies, the outflow model of the galaxy is described as having three components; mainly a narrow component, a secondary narrow component and a broad component, being blueshifted by -157 ± 33 kilometers per second, in relation to the narrow component. The broad and narrow components are estimated to have full-width at half maximum measurements of 386 ± 14 and 1,543 ± 34 kilometer per seconds.[11] There is also evidence of compact ionized nuclear outflows in the galaxy. with mass outflow rates of 20.1+72.9-14.9 Mʘ per year, and kinetic power of around 2.5 percent.[9]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 "NED search results for IRAS F17179+5444". https://ned.ipac.caltech.edu/byname?objname=IRAS+F17179+5444&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ 2.0 2.1 2.2 Dey, Subhrata; Goyal, Arti; Małek, Katarzyna; Díaz-Santos, Tanio (2024-04-25). "Radio-only and Radio-to-far-ultraviolet Spectral Energy Distribution Modeling of 14 ULIRGs: Insights into the Global Properties of Infrared Bright Galaxies". The Astrophysical Journal 966 (1): 61. doi:10.3847/1538-4357/ad2c93. ISSN 0004-637X. Bibcode: 2024ApJ...966...61D. 
  3. ↑ 3.0 3.1 Leech, K. J.; Rowan-Robinson, M.; Lawrence, A.; Hughes, J. D. (1994-03-15). "Optical structure of a large sample of ultraluminous IRAS galaxies". Monthly Notices of the Royal Astronomical Society 267 (2): 253–269. doi:10.1093/mnras/267.2.253. ISSN 0035-8711. https://watermark02.silverchair.com/mnras267-0253.pdf?token=AQECAHi208BE49Ooan9kkhW_Ercy7Dm3ZL_9Cf3qfKAc485ysgAAA1swggNXBgkqhkiG9w0BBwagggNIMIIDRAIBADCCAz0GCSqGSIb3DQEHATAeBglghkgBZQMEAS4wEQQMO1ecgsWxkgPuQpr5AgEQgIIDDgkEtloeBdTtDSYFjU5biYeioSQblnwD89T08lMSqycm4ZAsuvn4ME_8XBfdfiIsbI7ewFaO-m_IL7-M2u9ximr3lAD5V4YmWrWceyhHD5W8b0SJ1rsrqoToRXuj4-cXqRv1slDteIVWNf174fgBcCd4Kw_nkxINGmgw2Jiyw6eKSPY89rOLd6Vb3mOX9q9eTYOJWqHPRqLfdsLWWSlAAbYD4c-58GxrWkKZESH3X-hdrg30-QiHGmKO08yxcpXQOqZtm1CPp-QtByEeWQySrg6kKYOzajO-AOmyB1QMNppziZYljLtvj8zShm4PESAv661M9F78E-2IiPBnj75--Le9sDmQMjpeyiODnBKzjI_caB9W7iz0hPKt5FYS8IeLQdGT5rPu2z24G5p09cr9IN14_uLu_bTU1J6asgq4X2Bj21PUIBF7eN30XyEnSqbsA3MLWSkOk2j0PXLr-Mor1NArSJbDBY76DDdXZgBEIgDwIH1fd8hdHQGOqoe0FKZt-kHjyEZO74oY4lteRkjGNUnK-xvlSAS12tbf_MPFQV9Z3qvR4_f293P-NC9wbvtlBd0MuQIBSiJQX4LmrycKFyvKRAdIa3xQE3PCxGDyHzoxMvtCAjH5zyo1qYjHzT7sp4LMyEnIz9bqDqt7SpxUb9iHH6cRQC9WxW25e4xTiy9A7LFL1eCLiezB_jDLQXQoWwxtzVwhMsxtEidAxUyT4YQ0sRYmpul6KJ4pYOkRy4sPm2XycDa2_pOY3pVuJZ6CIYIYzoXlAqJxVOLasRC_qm8HN_89knXyyegwoaFoESg8VLlyyO4D12-TJizIrYPoKPVojF-bPyieaHAEpEeIYH1uK6UbU8v_98plh4gnyOqI_piNyZ_3qVk1WXfwxspxUi2ZSlwUDiRo8TMlylkkxzXKEzJGuJimbHoOwegvSeo0_Ulw-mXlMEK-2bMAxUfgveMxwaXjJjx9KT_ZELrx2QXOmyfw_3U4OExmx38tAIzTV1yUD8n_4OnoYyvDMG8AwE3vRMb0YZ2clLHn-8jU. 
  4. ↑ Davies, R.I.; Burston, A.; Ward, M.J. (January 2002). "Investigating the central engine of ultraluminous infrared galaxies: near infrared imaging". Monthly Notices of the Royal Astronomical Society 329 (2): 367–376. doi:10.1046/j.1365-8711.2002.04990.x. ISSN 0035-8711. Bibcode: 2002MNRAS.329..367D. 
  5. ↑ Veilleux, S.; Kim, D.-C.; Sanders, D. B. (December 2002). "Optical and Near-Infrared Imaging of the IRAS 1 Jy Sample of Ultraluminous Infrared Galaxies. II. The Analysis" (in en). The Astrophysical Journal Supplement Series 143 (2): 315–376. doi:10.1086/343844. ISSN 0067-0049. Bibcode: 2002ApJS..143..315V. 
  6. ↑ Tadhunter, C; Rodríguez Zaurín, J; Rose, M; Spence, R A W; Batcheldor, D; Berg, M A; Ramos Almeida, C; Spoon, H W W et al. (2018-05-05). "Quantifying the AGN-driven outflows in ULIRGs (QUADROS) – II. Evidence for compact outflow regions from HST [O III] imaging observations". Monthly Notices of the Royal Astronomical Society 478 (2): 1558–1569. doi:10.1093/mnras/sty1064. ISSN 0035-8711. 
  7. ↑ de Vries, N.; Snellen, I. a. G.; Schilizzi, R. T.; Mack, K.-H.; Kaiser, C. R. (May 2009). "VLBI observations of the CORALZ sample: young radio sources at low redshift" (in en). Astronomy and Astrophysics 498 (2): 641–659. doi:10.1051/0004-6361/200811145. ISSN 0004-6361. Bibcode: 2009A&A...498..641D. 
  8. ↑ Chandola, Yogesh; Sirothia, S. K.; Saikia, D. J. (2011-09-29). "H I absorption towards nearby compact radio sources". Monthly Notices of the Royal Astronomical Society 418 (3): 1787–1795. doi:10.1111/j.1365-2966.2011.19607.x. ISSN 0035-8711. Bibcode: 2011MNRAS.418.1787C. 
  9. ↑ 9.0 9.1 Spence, R A W; Tadhunter, C N; Rose, M; Rodríguez Zaurín, J (2018-05-07). "Quantifying the AGN-driven outflows in ULIRGs (QUADROS) III: measurements of the radii and kinetic powers of eight near-nuclear outflows". Monthly Notices of the Royal Astronomical Society 478 (2): 2438–2460. doi:10.1093/mnras/sty1046. ISSN 0035-8711. 
  10. ↑ Nandi, S.; Das, M.; Dwarakanath, K. S. (June 2021). "Tracing the evolution of ultraluminous infrared galaxies into radio galaxies with low frequency radio observations" (in en). Monthly Notices of the Royal Astronomical Society 503 (4): 5746–5762. doi:10.1093/mnras/stab275. ISSN 0035-8711. 
  11. ↑ Rodríguez Zaurín, J.; Tadhunter, C. N.; Rose, M.; Holt, J. (June 2013). "The importance of warm, AGN-driven outflows in the nuclear regions of nearby ULIRGs" (in en). Monthly Notices of the Royal Astronomical Society 432 (1): 138–166. doi:10.1093/mnras/stt423. ISSN 0035-8711. 




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