User:C messier/NGC 3516

{{Infobox galaxy

| name = NGC 3516

| image = NGC 3516.png

| image_size = 250px

| caption =NGC 3516 by Hubble Space Telescope

| credit = NASA/JPL-Caltech and Judy Schmidt

| epoch = J2000

| type = (R)SB(s)0^0^ {{cite web

| title=NASA/IPAC Extragalactic Database

| work=Results for NGC 3516

| url=http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=NGC+3516

| accessdate=2016-01-18 }}

| ra = {{RA|11|06|47.5}}

| dec = {{DEC|+72|34|07}}

| dist_ly = 165 ± 50 Mly (51.5 ± 15.1 Mpc)

| z = 0.008836 ± 0.000023

| h_radial_v = 2649 ± 7 km/s

| appmag_v = 11.5{{cite web |title=Revised NGC Data for NGC 3516 |url=http://spider.seds.org/ngc/revngcic.cgi?NGC3516 |website=spider.seds.org |accessdate=25 November 2018}}

| size_v = 1′.7 × 1′.3

| constellation name = Ursa Major

| notes = Seyfert galaxy

| names = UGC 6153, MCG +12-11-009, PGC 33623

}}

NGC 3516 is a barred lenticular galaxy in the constellation of Ursa Major. NGC 3516 is located about 150 million light years away from Earth, which means, given its apparent dimensions, that NGC 3516 is approximately 100,000 light years across. It was discovered by William Herschel on April 3, 1785.{{cite web |last1=Seligman |first1=Courtney |title=NGC 3516 |url= http://cseligman.com/text/atlas/ngc35.htm#3516 |website=Celestial Atlas |accessdate=19 November 2018}}

Characteristics

In 1943, this galaxy was one of six nebulae listed by American astronomer Carl Keenan Seyfert that showed broad emission lines in their nuclei. Members of this class of objects became known as Seyfert galaxies, and they were noted to have a higher than normal surface brightness in their nuclei. NGC 3516 is believed to host a supermassive black hole whose mass is estimated to be {{val|4.27|1.46|e=7}} {{solar mass|link=yes}} based on broad emission-line reverberation mapping{{cite journal

|doi=10.1007/s11214-013-9987-4

| title = Measuring the Masses of Supermassive Black Holes

| journal = Space Science Reviews

| volume = 183

| page = 253

| url = http://www.astronomy.ohio-state.edu/~peterson/Docs/petersonISSI.pdf

| year = 2013

| last1 = Peterson

| first1 = Bradley M.

| bibcode = 2014SSRv..183..253P

}} or {{val|23000000}} {{solar mass}} as measured based on velocity dispersion.{{cite journal|doi=10.1086/317314|title=Black Hole Mass, Velocity Dispersion, and the Radio Source in Active Galactic Nuclei|journal=The Astrophysical Journal|volume=544|issue=2|pages=L91|year=2000|last1=Nelson|first1=Charles H.|bibcode=2000ApJ...544L..91N|arxiv = astro-ph/0009188 }}

Due to its high brightness in both UV and X-rays, and its prominent and clear active galactic nucleus absorption features, it has been an ideal laboratory for studying the AGN warm-absorber outflows with high-resolution spectroscopy. Over the past few decades, there have been many UV and X-ray case studies of the ionized outflows in NGC 3516.{{cite journal |last1=Mehdipour |first1=Missagh |last2=Kriss |first2=Gerard A. |last3=Brenneman |first3=Laura W. |last4=Costantini |first4=Elisa |last5=Kaastra |first5=Jelle S. |last6=Branduardi-Raymont |first6=Graziella |last7=Di Gesu |first7=Laura |last8=Ebrero |first8=Jacobo |last9=Mao |first9=Junjie |title=Changing-look Event in NGC 3516: Continuum or Obscuration Variability? |journal=The Astrophysical Journal |date=1 January 2022 |volume=925 |issue=1 |pages=84 |doi=10.3847/1538-4357/ac42ca}} NGC 3516 has been a remarkably variable AGN, showing changes in both the intrinsic continuum{{cite journal |last1=Ilić |first1=D. |last2=Oknyansky |first2=V. |last3=Popović |first3=L. č. |last4=Tsygankov |first4=S. S. |last5=Belinski |first5=A. A. |last6=Tatarnikov |first6=A. M. |last7=Dodin |first7=A. V. |last8=Shatsky |first8=N. I. |last9=Ikonnikova |first9=N. P. |last10=Rakić |first10=N. |last11=Kovačević |first11=A. |last12=Marčeta-Mandić |first12=S. |last13=Burlak |first13=M. A. |last14=Mishin |first14=E. O. |last15=Metlova |first15=N. V. |last16=Potanin |first16=S. A. |last17=Zheltoukhov |first17=S. G. |title=A flare in the optical spotted in the changing-look Seyfert NGC 3516 |journal=Astronomy & Astrophysics |date=June 2020 |volume=638 |pages=A13 |doi=10.1051/0004-6361/202037532}} and the intrinsic absorption by the ionized outflows.{{cite journal |last1=Dunn |first1=Jay P. |last2=Parvaresh |first2=Rozhin |last3=Kraemer |first3=S. B. |last4=Crenshaw |first4=D. Michael |title=Evolution of the Outflows in NGC 3516 |journal=The Astrophysical Journal |date=23 February 2018 |volume=854 |issue=2 |pages=166 |doi=10.3847/1538-4357/aaa95d}} In 2014, the broad lines almost disappeared, probably becoming obstructed, and thus the galaxy has been identified as a changing-look AGN, meaning it changed spectra between type 1 and type 2 AGN.{{cite journal |last1=Shapovalova |first1=A I |last2=Popović |first2=L č |last3=Afanasiev |first3=V L |last4=Ilić |first4=D |last5=Kovačević |first5=A |last6=Burenkov |first6=A N |last7=Chavushyan |first7=V H |last8=Marčeta-Mandić |first8=S |last9=Spiridonova |first9=O |last10=Valdes |first10=J R |last11=Bochkarev |first11=N G |last12=Patiño-Álvarez |first12=V |last13=Carrasco |first13=L |last14=Zhdanova |first14=V E |title=Long-term optical spectral monitoring of a changing-look active galactic nucleus NGC 3516 – I. Continuum and broad-line flux variability |journal=Monthly Notices of the Royal Astronomical Society |date=1 June 2019 |volume=485 |issue=4 |pages=4790–4803 |doi=10.1093/mnras/stz692}}

The galaxy has been found to emit radiowaves, with the source extending towards the north for about 0.65 arcseconds.{{cite journal |last1=Nagar |first1=Neil M. |last2=Wilson |first2=Andrew S. |last3=Mulchaey |first3=John S. |last4=Gallimore |first4=Jack F. |title=Radio Structures of Seyfert Galaxies. VIII. A Distance‐ and Magnitude‐Limited Sample of Early‐Type Galaxies |journal=The Astrophysical Journal Supplement Series |date=February 1999 |volume=120 |issue=2 |pages=209–245 |doi=10.1086/313183}} That structure is a bit curved and probably is related to the gaseous outflow.{{cite journal |last1=Miyaji |first1=Takamitsu |last2=Wilson |first2=Andrew S. |last3=Perez-Fournon |first3=Ismael |title=The radio source and bipolar nebulosity in the Seyfert galaxy NGC 3516 |journal=The Astrophysical Journal |date=January 1992 |volume=385 |pages=137 |doi=10.1086/170922}} A spiral dust feature measuring 3 arcseconds in diameter is visible north of the nucleus. A blue filamentary feature is visible northeast of the nucleus and another blue feature is visible 1.5 arcseconds southwest of the nucleus.{{cite journal |last1=Regan |first1=Michael W. |last2=Mulchaey |first2=John S. |title=Using HUBBLE SPACE TELESCOPE Imaging of Nuclear Dust Morphology to Rule Out Bars Fueling Seyfert Nuclei |journal=The Astronomical Journal |date=June 1999 |volume=117 |issue=6 |pages=2676–2694 |doi=10.1086/300888}}

Nearby galaxies

NGC 3516 is a relatively isolated galaxy. Near galaxies include NGC 3147 with its group that NGC 3155, UGC 5570, UGC 5686, and UGC 5689, NGC 3183, NGC 3348, and NGC 3364.{{cite journal|last1=Makarov|first1=Dmitry|last2=Karachentsev|first2=Igor|title=Galaxy groups and clouds in the local (z∼ 0.01) Universe|journal=Monthly Notices of the Royal Astronomical Society|date=21 April 2011|volume=412|issue=4|pages=2498–2520|doi=10.1111/j.1365-2966.2010.18071.x|url=http://www.sao.ru/hq/dim/groups/galaxies.dat|bibcode=2011MNRAS.412.2498M|arxiv = 1011.6277 }} Garcia identified NGC 3516 as a member of group that also includes the galaxies NGC 3348, and NGC 3364.{{cite journal |last1=Garcia |first1=A. M. |title=General study of group membership. II. Determination of nearby groups. |journal=Astronomy and Astrophysics Supplement Series |date=1 July 1993 |volume=100 |pages=47–90 |url=https://cdsarc.cds.unistra.fr/ftp/J/A+AS/100/47/table2.dat |bibcode= 1993A&AS..100...47G |issn=0365-0138}}