3C 449

{{Short description|Radio galaxy in the constellation Lacerta}}

{{Infobox Galaxy

| name = 3C 449

| image = 3C_449_PanSTARRS_i.r.g.jpg

| epoch = J2000

| ra = {{RA|22|31|20.55}}{{cite web

| title=NASA/IPAC Extragalactic Database

| work=Results for 3C 449

| url=http://nedwww.ipac.caltech.edu/

| access-date=2006-10-26 }}

| dec = {{DEC|+39|21|29.6}}

| constellation name = Lacerta

| z = 0.01711

| dist_ly = 213 Mly

| type = E/S0

| appmag_v = 12.35

| size_v = 1.05{{prime}}×0.74{{prime}}

| names = UGC 12064, 3C 449, 4C 39.69, LEDA 69055, B2229+390

}}

3C 449 is a low-redshift (z = 0.017) Fanaroff and Riley class I radio galaxy. It is thought to contain a highly warped circumnuclear disk surrounding the central active galactic nucleus (AGN).{{cite journal |last1=Tremblay |first1=Grant R. |last2=Quillen |first2=Alice C. |last3=Floyd |first3=David J. E. |last4=Noel-Storr |first4=Jacob |last5=Baum |first5=Stefi A. |last6=Axon |first6=David |last7=O’Dea |first7=Christopher P. |last8=Chiaberge |first8=Marco |last9=Macchetto |first9=F. Duccio |last10=Sparks |first10=William B. |last11=Miley |first11=George K. |last12=Capetti |first12=Alessandro |last13=Madrid |first13=Juan P. |last14=Perlman |first14=Eric |title=The Warped Nuclear Disk of Radio Galaxy 3C 449 |journal=The Astrophysical Journal |date=20 May 2006 |volume=643 |issue=1 |pages=101–111 |doi=10.1086/502643|arxiv=astro-ph/0510650 |bibcode=2006ApJ...643..101T |hdl=1802/2874 |s2cid=16067609 |hdl-access=free }} The name signifies that it was the 449th object (ordered by right ascension) of the Third Cambridge Catalog of Radio Sources (3C), published in 1959.

When observed by the Very Large Array, the galaxy features two symmetrical radio jets that end up in lobes and an unresolved core. The jets are relativistic near the core, but their speed is greatly reduced at about 10 arcseconds (which corresponds to about 5 kiloparsecs at the distance of the galaxy) from the core. The lobes appear complex, with plumes and wiggles. The north lobe is elongated while the end of the south lobe is round. The total apparent size of the radio features is about 30 arcminutes.{{cite journal |last1=Feretti |first1=L. |last2=Perley |first2=R. |last3=Giovannini |first3=G. |last4=Andernach |first4=H. |title=VLA observations of the giant radio galaxy 3C 449 |journal=Astronomy and Astrophysics |date=1 January 1999 |volume=341 |pages=29–43 |arxiv=astro-ph/9810305 |bibcode=1999A&A...341...29F |url=https://articles.adsabs.harvard.edu/pdf/1999A%26A...341...29F |issn=0004-6361}} Both lobes are leaning towards the west, indicating they are pushed that way by external gas which was formed during a galaxy merger the last 1.3 – 1.6 billion years.{{cite journal |last1=Lal |first1=Dharam V. |last2=Kraft |first2=Ralph P. |last3=Randall |first3=Scott W. |last4=Forman |first4=William R. |last5=Nulsen |first5=Paul E. J. |last6=Roediger |first6=Elke |last7=ZuHone |first7=John A. |last8=Hardcastle |first8=Martin J. |last9=Jones |first9=Christine |last10=Croston |first10=Judith H. |title=Gas Sloshing and Radio Galaxy Dynamics in the Core of the 3C 449 Group |journal=The Astrophysical Journal |date=29 January 2013 |volume=764 |issue=1 |pages=83 |doi=10.1088/0004-637X/764/1/83|arxiv=1210.7563 |bibcode=2013ApJ...764...83L |hdl=2060/20140000251 |s2cid=118548355 |hdl-access=free }}

3C 449 is the most prominent member of the Zwicky 2231.2+3732 galaxy cluster. The halo of 3C 449 is connected via a bridge with another galaxy located 37 arcseconds to the north.{{cite journal |last1=Martel |first1=André R. |last2=Baum |first2=Stefi A. |last3=Sparks |first3=William B. |last4=Wyckoff |first4=Eric |last5=Biretta |first5=John A. |last6=Golombek |first6=Daniel |last7=Macchetto |first7=Ferdinando D. |last8=de Koff |first8=Sigrid |last9=McCarthy |first9=Patrick J. |last10=Miley |first10=George K. |title=Hubble Space Telescope Snapshot Survey of 3CR Radio Source Counterparts. III. Radio Galaxies with [FORMULA][F]z |journal=The Astrophysical Journal Supplement Series |date=May 1999 |volume=122 |issue=1 |pages=81–108 |doi=10.1086/313205|doi-access=free }}