dc.contributor.author |
Cho, Hojin |
|
dc.contributor.author |
Woo, Jong-Hak |
|
dc.contributor.author |
Hodges-Kluck, E |
|
dc.contributor.author |
Son, Donghoon |
|
dc.contributor.author |
Shin, Jaejin |
|
dc.contributor.author |
Gallo, Elena |
|
dc.contributor.author |
Bae, Hyun-Jin |
|
dc.contributor.author |
Brink, T. G |
|
dc.contributor.author |
Cho, Wanjin |
|
dc.contributor.author |
Filippenko, A. V |
|
dc.contributor.author |
Horst, J. C |
|
dc.contributor.author |
Ilic, Dragana |
|
dc.contributor.author |
Joner, M. D |
|
dc.contributor.author |
Kang, Daeun |
|
dc.contributor.author |
Kang, Wonseok |
|
dc.contributor.author |
Kaspi, Shai |
|
dc.contributor.author |
Kim, Taewoo |
|
dc.contributor.author |
Kovacevic, A. B |
|
dc.contributor.author |
Kumar, S |
|
dc.contributor.author |
Le, Huynh Anh N |
|
dc.contributor.author |
Nadzhip, A. E |
|
dc.contributor.author |
Nunez, F. P |
|
dc.contributor.author |
Metlov, V. G |
|
dc.contributor.author |
Oknyansky, V. L |
|
dc.contributor.author |
Park, Songyoun |
|
dc.contributor.author |
Popovic, L. C |
|
dc.contributor.author |
Rakshit, S |
|
dc.contributor.author |
Schramm, M |
|
dc.contributor.author |
Shatsky, N. I |
|
dc.contributor.author |
Spencer, M |
|
dc.contributor.author |
Sung, E.-H |
|
dc.contributor.author |
Sung, H.-i |
|
dc.contributor.author |
Tatarnikov, A. M |
|
dc.contributor.author |
Vince, O |
|
dc.date.accessioned |
2021-02-14T06:08:03Z |
|
dc.date.available |
2021-02-14T06:08:03Z |
|
dc.date.issued |
2020-04-01 |
|
dc.identifier.citation |
The Astrophysical Journal, Vol. 892, No. 2, 93 |
en_US |
dc.identifier.issn |
0004-637X |
|
dc.identifier.uri |
http://hdl.handle.net/2248/7640 |
|
dc.description |
Restricted Access |
en_US |
dc.description.abstract |
We present a variability study of the lowest-luminosity Seyfert 1 nucleus of the galaxy NGC 4395 based on
photometric monitoring campaigns in 2017 and 2018. Using 22 ground-based and space telescopes, we monitored
NGC 4395 with a ∼5-minute cadence during a period of 10 days and obtained light curves in the ultraviolet (UV),
V, J, H, and K/Ks bands, as well as narrowband Hα. The rms variability is ∼0.13 mag in the Swift UVM2 and V
filter light curves, decreasing down to ∼0.01 mag in the K filter. After correcting for the continuum contribution to
the Hα narrow band, we measured the time lag of the Hα emission line with respect to the V-band continuum as
-
+ 55 31
27– -
+ 122 67
33 minutes in 2017 and -
+ 49 14
15– -
+ 83 14
13 minutes in 2018, depending on assumptions about the continuum
variability amplitude in the Hα narrow band. We obtained no reliable measurements for the continuum-tocontinuum lag between UV and V bands and among near-IR bands, owing to the large flux uncertainty of UV
observations and the limited time baseline. We determined the active galactic nucleus (AGN) monochromatic
luminosity at 5100 Å, l l =´ ( ) - L 5.75 0.40 10 erg s 39 1, after subtracting the contribution of the nuclear star
cluster. While the optical luminosity of NGC 4395 is two orders of magnitude lower than that of other
reverberation-mapped AGNs, NGC 4395 follows the size–luminosity relation, albeit with an offset of 0.48 dex
(>2.5σ) from the previous best-fit relation of Bentz et al |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
IOP Publishing |
en_US |
dc.relation.uri |
https://doi.org/10.3847/1538-4357/ab7a98 |
|
dc.rights |
© The American Astronomical Society |
|
dc.subject |
Reverberation mapping |
en_US |
dc.subject |
Active galactic nuclei |
en_US |
dc.subject |
Active galaxies |
en_US |
dc.subject |
Galaxy nuclei |
en_US |
dc.subject |
Low-luminosity active galactic nuclei |
en_US |
dc.subject |
Intermediate-mass black holes |
en_US |
dc.subject |
Seyfert galaxies |
en_US |
dc.title |
Variability and the Size–Luminosity Relation of the Intermediate-mass AGN in NGC 4395 |
en_US |
dc.type |
Article |
en_US |