UGC 9684

UGC 9684
Hubble Space Telescope image of UGC 9684
Observation data (J2000 epoch)
ConstellationBoötes
Right ascension15h 03m 50.477s
Declination+42d 06m 55.55s
Redshift0.016866
Heliocentric radial velocity5,056 km/s
Distance247 Mly (75.7 Mpc)
Apparent magnitude (V)14.4
Characteristics
TypeSBab, Sab
Size90,000 ly
Apparent size (V)1.35 x 0.56 arcmin
Other designations
PGC 53758, ECO 04872, CGCG 221-023, MCG +07-31-024, 2MASX J15035050+4206556, 2MASS J15035049+4206554, SDSS J150350.47+420655.5, IRAS F15020+4218, UZC J150350.5+420655, LEDA 53758

UGC 9684 is a barred spiral galaxy with a ring structure[1] in the Boötes constellation.[2] It is located 250 million light-years from the Solar System and has an approximate diameter of 90,000 light-years.[3]

The luminosity class of UGC 9684 is I-II[4][3] and it is classified as an active star-forming galaxy according to a study published in 2022,[5] in which produces one solar mass of stars every few years, with levels of stellar formation.[6]

Studying of star formation rate for UGC 9684

Scientists who studied UGC 9684, have longed to find out the star-formation rate for UGC 9684.[5] To do this, they used a Fitting and Assessment of Synthetic Templates code.[7] The scientists used further observations via ultraviolet, both optical and near-infrared and from the luminosity measurements from different databases from GALEX,[8] SDSS and from the final release of the MASS extended source catalog by Jarrett et al. 2000,[9] with all the data retrieved from NASA/IPAC Extragalactic Database.[5]

As for the star formation, they employed a decreasing function of (SFR ∝ e−t ) and also a delayed function (SFR ∝ t × e−t ) as well as the stellar population libraries written from Bruzual & Charlot[10] and Convoy et al.[11] Several metallicity estimates, published by Prieto et al. 2008,[12] Kelly & Kirshner from 2012,[13] whom the majority agreed, it is slightly above solar oxygen abundance 12+ log(O/H) ≈ 9.0 which corresponds to ~2 Z⊙.[5]

Scientists therefore found that the star-formation rate of UGC 9684 is 0.25–0.39 M⊙ yr−1.[5] Apart from that, they found the total stellar mass for the galaxy is M⋆ = (2.0–3.5) × 1010 M⊙ which is a current specific of SFR sSFR ≈ 0.01 Gyr−1. This is higher compared to literature but compatible to large number of recent events in UGC 9684.[5]

Supernovae

Three supernovae and one astronomical transient have been discovered in UGC 9684: SN 2006ed, SN 2012ib, AT 2017cgh, and SN 2020pni. This makes it as one of the most active supernova-producing galaxies.[6]

SN 2006ed

SN 2006ed was discovered on September 18, 2006, via unfiltered CCD images, by N. Joubert, D. R. Madison, R. Mostardi, H. Khandrika and W. Li from University of California, Berkeley on behalf of Lick Observatory Supernova Search program (LOSS). SN 2006ed had a magnitude on 19.0.[14] It was located 1".8 east and 7".2 south of the nucleus.[15] This supernova was Type II.[16][14]

SN 2012ib

SN 2012ib was discovered on December 20, 2012, by amateur astronomer, V. Shumkov from Sternberg Astronomical Institute (SAI), on four 60-sec unfiltered images from the MASTER-Amur robotic telescope via a 0.40-m f/2.5 reflector.[17] The supernova was located at 48".7 east and 0".4 south of the nucleus, which it had a magnitude of 18.9.[18] The supernova was Type Ib/c.[19]

AT 2017cgh

AT 2017cgh was discovered on March 15, 2017, by Pan-STARRS1[20] Science consortium.[21] It was located 0".0 east and 0".0 north of the nucleus with a magnitude of 17.7.[21] This astronomical transient had an unknown type, and was never officially classified as a supernova.[22]

SN 2020pni

SN 2020pni was discovered on July 16, 2020, by a team of astronomers on behalf of the ALeRCE broker[23] via r-ZTF filters which was taken by a Palomar 1.2m Oachin telescope.[24] It was located 5".7 west and 5".0 south of the nucleus with a magnitude of 17.0.[25] The supernova was Type II[26] in which its progenitor, a massive star,[27] was enriched in helium and nitrogen in relative abundances in mass fractions of 0.30–0.40 and 8.2 × 10−3, respectively.[5]

A first study shows 1 day after the discovery, there is a significant He II emission which has strong flash features.[28] Another study shows during the 4 days after, there was an increase in velocity of hydrogen lines (from ~250 to ~1000 km/s) suggesting complex circumstellar medium (CSM).[5] A presence of dense and confined CSM as well as its inhomogeneous structure, indicates a phrase of enhanced mass loss of the SN 2020pni progenitor a year before the explosion.[5] As of 2023, the supernova has since faded from view.[6]

References

  1. ^ "HyperLeda -object description". atlas.obs-hp.fr. Retrieved 2024-05-07.
  2. ^ Ford, Dominic. "UGC 9684 (Galaxy)". In-The-Sky.org. Retrieved 2024-05-07.
  3. ^ a b "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-05-07.
  4. ^ "Reference Lookup | NASA/IPAC Extragalactic Database". ned.ipac.caltech.edu. Retrieved 2024-05-07.
  5. ^ a b c d e f g h i Terreran, G.; Jacobson-Galán, W. V.; Groh, J. H.; Margutti, R.; Coppejans, D. L.; Dimitriadis, G.; Kilpatrick, C. D.; Matthews, D. J.; Siebert, M. R.; Angus, C. R.; Brink, T. G.; Filippenko, A. V.; Foley, R. J.; Jones, D. O.; Tinyanont, S. (February 2022). "The Early Phases of Supernova 2020pni: Shock Ionization of the Nitrogen-enriched Circumstellar Material". The Astrophysical Journal. 926 (1): 20. arXiv:2105.12296. Bibcode:2022ApJ...926...20T. doi:10.3847/1538-4357/ac3820. ISSN 0004-637X.
  6. ^ a b c [email protected]. "A star forming factory". www.spacetelescope.org. Retrieved 2024-05-07.
  7. ^ Kriek, Mariska; Dokkum, Pieter G. van; Labbé, Ivo; Franx, Marijn; Illingworth, Garth D.; Marchesini, Danilo; Quadri, Ryan F. (July 2009). "An Ultra-Deep Near-Infrared Spectrum of a Compact Quiescent Galaxy at z = 2.2". The Astrophysical Journal. 700 (1): 221. arXiv:0905.1692. Bibcode:2009ApJ...700..221K. doi:10.1088/0004-637X/700/1/221. ISSN 0004-637X.
  8. ^ Seibert, Mark; Wyder, T.; Neill, J.; Madore, B.; Bianchi, L.; Smith, M.; Shiao, B.; Schiminovich, D.; Rich, R. M.; Conrow, T.; Martin, D. C.; GALEX Catalog Team (2012-01-01). "The Galaxy Evolution Explorer (GALEX) Source Catalogs". American Astronomical Society Meeting Abstracts #219. 219: 340.01. Bibcode:2012AAS...21934001S.
  9. ^ Jarrett, T. H.; Chester, T.; Cutri, R.; Schneider, S.; Skrutskie, M.; Huchra, J. P. (2000-05-01). "2MASS Extended Source Catalog: Overview and Algorithms". The Astronomical Journal. 119 (5): 2498–2531. arXiv:astro-ph/0004318. Bibcode:2000AJ....119.2498J. doi:10.1086/301330. ISSN 0004-6256.
  10. ^ Bruzual, G.; Charlot, S. (October 1, 2003). "Stellar population synthesis at the resolution of 2003". academic.oup.com. Retrieved 2024-05-12.
  11. ^ Conroy, Charlie; Gunn, James E.; White, Martin (2009-06-12). "The Propagation of Uncertainties in Stellar Population Synthesis Modeling. I. The Relevance of Uncertain Aspects of Stellar Evolution and the Initial Mass Function to the Derived Physical Properties of Galaxies". The Astrophysical Journal. 699 (1): 486–506. arXiv:0809.4261. Bibcode:2009ApJ...699..486C. doi:10.1088/0004-637x/699/1/486. ISSN 0004-637X.
  12. ^ Prieto, Jose L.; Stanek, Krzysztof Z.; Beacom, John F. (February 2008). "Characterizing Supernova Progenitors via the Metallicities of their Host Galaxies, from Poor Dwarfs to Rich Spirals". The Astrophysical Journal. 673 (2): 999–1008. arXiv:0707.0690. Bibcode:2008ApJ...673..999P. doi:10.1086/524654. ISSN 0004-637X.
  13. ^ Kelly, Patrick L.; Kirshner, Robert P. (2012-10-26). "Core-Collapse Supernovae and Host Galaxy Stellar Populations". The Astrophysical Journal. 759 (2): 107. arXiv:1110.1377. Bibcode:2012ApJ...759..107K. doi:10.1088/0004-637x/759/2/107. ISSN 0004-637X.
  14. ^ a b Joubert, N.; Li, W. (2006-08-01). "Supernovae 2006ed, 2006ee, 2006ef". Central Bureau Electronic Telegrams. 597: 1. Bibcode:2006CBET..597....1J.
  15. ^ "Bright Supernovae - 2006". www.rochesterastronomy.org. Retrieved 2024-05-07.
  16. ^ "SN 2006ed | Transient Name Server". www.wis-tns.org. Retrieved 2024-05-07.
  17. ^ Lipunov, V.; Shumkov, V.; Denisenko, D.; Gorbovskoy, E.; Brimacombe, J.; Tomasella, L.; Benetti, S.; Cappellaro, E.; Ochner, P.; Pastorello, A.; Turatto, M. (2012-12-01). "Supernova 2012ib in UGC 9684 = Psn J15035487+4206553". Central Bureau Electronic Telegrams. 3359: 1. Bibcode:2012CBET.3359....1L.
  18. ^ [email protected]. "Bright Supernovae - 2012". www.rochesterastronomy.org. Retrieved 2024-05-07.
  19. ^ "SN 2012ib | Transient Name Server". www.wis-tns.org. Retrieved 2024-05-07.
  20. ^ Chambers, K. C.; Huber, M. E.; Flewelling, H.; Magnier, E. A.; Primak, N.; Schultz, A.; Smartt, S. J.; Smith, K. W.; Tonry, J.; Waters, C.; Wright, D. E.; Young, D. R. (2017-01-01). "Pan-STARRS1 Transient Discovery Report for 2017-01-03". Transient Name Server Discovery Report. 2017–14: 1. Bibcode:2017TNSTR..14....1C.
  21. ^ a b "Bright Supernovae - 2017". www.rochesterastronomy.org. Retrieved 2024-05-07.
  22. ^ "AT 2017cgh | Transient Name Server". www.wis-tns.org. Retrieved 2024-05-07.
  23. ^ "Home | ALeRCE". alerce.science. Retrieved 2024-05-07.
  24. ^ "Discovery certificate for object 2020pni | Transient Name Server". www.wis-tns.org. Retrieved 2024-05-07.
  25. ^ "Bright Supernovae - 2020". www.rochesterastronomy.org. Retrieved 2024-05-07.
  26. ^ "SN 2020pni | Transient Name Server". www.wis-tns.org. Retrieved 2024-05-07.
  27. ^ Martinez, L.; Bersten, M. C.; Anderson, J. P.; González-Gaitán, S.; Förster, F.; Folatelli, G. (2020-10-01). "Progenitor properties of type II supernovae: fitting to hydrodynamical models using Markov chain Monte Carlo methods". Astronomy & Astrophysics. 642: A143. arXiv:2008.05572. Bibcode:2020A&A...642A.143M. doi:10.1051/0004-6361/202038393. ISSN 0004-6361.
  28. ^ Bruch, R.; Nordin, J.; Schulze, S.; Yang, Y.; Irani, I.; Gal-Yam, A.; Yaron, O.; Perley, D.; Sollerman, J. (2020-07-01). "ZTF early discovery and rapid follow-up of the infant SN ZTF20ablygyy/2020pni". Transient Name Server AstroNote. 136: 1. Bibcode:2020TNSAN.136....1B.