Tri-dimensional Spectroscopy of the Seyfert Galaxy NGC 1275: Kinematics and Excitation of the Cooling-Flow Gas

NGC 1275, the Perseus cluster cD galaxy, is a well-known Seyfert 1 galaxy and also one of the strongest extragalactic radio sources (3C84). Although many studies have been done on the extended optical emission-line region of NGC 1275, which is thought to be associated with the X-ray cooling-flow phenomenon (e.g., Heckman et al. 1989, Ferruit and Pecontal 1994), the excitation mechanism of the emission-line gas and two-dimensional gas kinematics are still unclear. We made tri-dimensional spectroscopy of NGC 1275 in order to reveal two-dimensional kinematics and- the relation between the gas motion and the excitation of the emission lines.

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X-ray and optical emission-line filaments in the cooling flow cluster 2A 0335 + 096

The Astrophysical Journal ◽

10.1086/186537 ◽

1992 ◽

Vol 397 ◽

pp. L31 ◽

Cited By ~ 18

Author(s):

Craig L. Sarazin ◽

Robert W. O'Connell ◽

Brian R. McNamara

Keyword(s):

Emission Line ◽

Optical Emission ◽

X Ray ◽

Cooling Flow

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Radially Inflowing Molecular Gas in NGC 1275 Deposited by an X‐Ray Cooling Flow in the Perseus Cluster

The Astrophysical Journal ◽

10.1086/523664 ◽

2008 ◽

Vol 672 (1) ◽

pp. 252-265 ◽

Cited By ~ 48

Author(s):

Jeremy Lim ◽

YiPing Ao ◽

Dinh‐V‐Trung

Keyword(s):

Molecular Gas ◽

X Ray ◽

Cooling Flow ◽

Ngc 1275 ◽

Perseus Cluster

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X-ray Imaging Studies of NGC 1275 and the Core of the Perseus Cluster

Highlights of Astronomy ◽

10.1007/978-94-015-6912-5_96 ◽

1980 ◽

pp. 741-745

Author(s):

J. Grindlay ◽

G. Branduardi ◽

A. Fabian

Keyword(s):

Imaging Studies ◽

X Ray ◽

The Core ◽

X Ray Imaging ◽

Ngc 1275 ◽

Perseus Cluster

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The X-Ray Nova GRO J0422+32 in Decline and Quiescence

International Astronomical Union Colloquium ◽

10.1017/s0252921100039245 ◽

1996 ◽

Vol 158 ◽

pp. 399-400

Author(s):

M. R. Garcia ◽

P. J. Callanan ◽

J. E. McClintock ◽

P. Zhao

Keyword(s):

Emission Line ◽

Emission Region ◽

Dwarf Novae ◽

X Ray ◽

First Order ◽

Band Emission ◽

Line Region ◽

Hα Emission ◽

The Stability ◽

The Continuum

We have followed the X-ray nova GRO J0422+32, spectroscopically and photometrically, throughout the decline to quiescence.In the final stages of decay (days 430…880 after the outburst, see Callanan et al. (1995) for the epoch 1995), the equivalent width (EW) of the Hα emission increases monotonically and the R magnitude decreases monotonically. This suggests that the flux in the Hα line is constant, while the continuum fades. The Hα flux is the product of the R band flux (F(R), arbitrarily scaled to 100 at R = 19 mag) and the EW, and is shown in the last column of the table below. The Hα flux varies by only ~ 30% while the continuum fades by a factor of eight (from R = 19 mag to R = 21.3 mag). So, to first order, the Hα luminosity is constant in the final stages of decay. While it is generally the case that the emission line EWs in individual dwarf novae also increase during the decay, the exact behavior seen in GRO J0422+32 is not what is seen for dwarf novae (on average). Using the relation between EW[Hβ] and Mv given in figure 6 of Patterson (1984), we would expect a factor of ~ 5 variation in the Hα flux during days 430…880. The stability of the Hα flux implies that somehow the emission line region is ‘disconnected’ from the continuum (R–band) emission region.

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High Velocity Outflow in the Extended Emission-Line Region of the Seyfert Galaxy NGC 7319

The Astronomical Journal ◽

10.1086/117767 ◽

1996 ◽

Vol 111 ◽

pp. 140 ◽

Cited By ~ 16

Author(s):

Kentaro Aoki ◽

Hiroshi Ohtani ◽

Michitosh Yoshida ◽

George Kosugi

Keyword(s):

Emission Line ◽

High Velocity ◽

Seyfert Galaxy ◽

Line Region ◽

Extended Emission

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X-ray and Gamma-ray Variability of NGC 1275

Galaxies ◽

10.3390/galaxies8030063 ◽

2020 ◽

Vol 8 (3) ◽

pp. 63

Author(s):

Varsha Chitnis ◽

Amit Shukla ◽

K. P. Singh ◽

Jayashree Roy ◽

Sudip Bhattacharyya ◽

...

Keyword(s):

Time Scales ◽

Gamma Ray ◽

Radio Galaxy ◽

Cluster Emission ◽

X Ray ◽

Gamma Ray Emission ◽

High Degree ◽

Ngc 1275 ◽

Perseus Cluster ◽

Very High

Gamma-ray emission from the bright radio source 3C 84, associated with the Perseus cluster, is ascribed to the radio galaxy NGC 1275 residing at the centre of the cluster. Study of the correlated X-ray/gamma-ray emission from this active galaxy, and investigation of the possible disk-jet connection, are hampered because the X-ray emission, particularly in the soft X-ray band (2–10 keV), is overwhelmed by the cluster emission. Here we present a method to spectrally decouple the cluster and active galactic nucleus (AGN) emission in imaging X-ray detectors. We use three sets of simultaneous Niel Gehrels Swift XRT and NuStar data. These observations were made during the period 2015 November to 2017 February, when a huge increase in the gamma-ray emission was observed. We find that the gamma-ray emission shows a very high degree of variability (40%–50%) on time scales of 1–10 days, whereas the hard X-ray emission, associated with the AGN, shows a low variability (∼15%–30%), on various time scales in the range of 0.01–60 days.

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