IC 3528
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| IC 3528 | |
|---|---|
 | |
| Observation data (J2000 epoch) | |
| Constellation | Coma Berenices |
| Right ascension | 12h 34m 55.90s |
| Declination | +15° 33′ 56.2″ |
| Redshift | 0.04582 0.00004 |
| Heliocentric radial velocity | 13,773 km/s |
| Distance | 657 Mly (201.43 Mpc) |
| Apparent magnitude (V) | 14.6 |
| Apparent magnitude (B) | 15.4 |
| Characteristics | |
| Type | SAB(r)b, Sy 1.5 |
| Size | 0.40' x 0.4' |
| Notable features | Seyfert Galaxy |
| Other designations | |
| PGC 41882, GSC 01446-00639, 2MASX J12345592+1533561, VCC 1593, Z 99-95, NVSS B123244+155026, ALFALFA 1-358, AGC 220811, SDSS J123455.90+153356.2, FAUST 3256, [HB91] 1232+158, LEDA 41882 | |
IC 3528 is spiral galaxy located 660 million light-years[1] away in the constellation of Coma Berenices.[2] It lies near to another spiral galaxy NGC 4540, although the two of them are quite far.[3][4] The object was discovered by Royal Harwood Frost on May 7, 1904.[5] Although listed as a member in the Virgo Cluster Catalogue[6] as VCC 1593, it is not a member of the Virgo cluster but a background galaxy.[7]
Starburst activity
IC 3528 is classified a narrow-line Seyfert 1.5 type galaxy.[8][9] Containing X-ray emission,[10] the galaxy shows strong evidence of non-gravitational outflow kinematics in its [O III] λ5007 emission feature.[11] In addition, IC 4528 contains broad emission lines with widths measuring Hβ FWHM ≤ 2000 km s−1 and is a type-1 active galactic nucleus (AGN) hosted inside a lower-luminosity galaxy that is found having a higher incidence of pseudo-bulges, with barred morphology, and considered less disturbed. This suggests narrow-line Type 1 AGNs like in the case of IC 3528, experiences a more quiescent evolutionary history that is driven primarily by internal secular evolution rather than external dynamical perturbations.[12]
IC 3528 has an estimated star formation rate of ≳6 M☉ yr−1[13] It is a dusty starburst galaxy exhibiting a strong Hδ line in absorption and modest [O II] emission, whom researchers found the galaxy is affected by reddening. Based on star formation rates derived from the FIR luminosities with the estimates based on the Hα line, they found the values obtained from these optical emission lines in IC 3528 are a factor of 10-70 (Hα) and 20-140 ([O II]) lower than the FIR estimates (50-300 Msolar yr−1).[14]
Metallicity
IC 3528 has a low gas fraction and higher oxygen abundance, making a it gas-poor galaxy and metal-rich, which demonstrates the idea that removal of gas from the outskirts of spirals increases the observed average metallicity by ~0.1 dex.[15]
