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Artículos de revistas sobre el tema "NGC 1386"

Autor: Grafiati

Publicado: 10 de marzo de 2023

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1

Ruschel-Dutra, Daniel, Miriani Pastoriza, Rogério Riffel, Dinalva A. Sales y Cláudia Winge. "A mid-IR comparative analysis of the Seyfert galaxies NGC 7213 and NGC 1386". Monthly Notices of the Royal Astronomical Society 438, n.º 4 (20 de enero de 2014): 3434–42. http://dx.doi.org/10.1093/mnras/stt2448.

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2

Iyomoto, Naoko, Kazuo Makishima, Yasushi Fukazawa, Makoto Tashiro y Yoshitaka Ishisaki. "Detection of Strong Fe-K Lines from the Spiral Galaxies NGC 1365 and NGC 1386". Publications of the Astronomical Society of Japan 49, n.º 4 (1 de agosto de 1997): 425–34. http://dx.doi.org/10.1093/pasj/49.4.425.

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3

Bennert, N., B. Jungwiert, S. Komossa, M. Haas y R. Chini. "Size and properties of the NLR in the Seyfert-2 galaxy NGC 1386". Astronomy & Astrophysics 446, n.º 3 (20 de enero de 2006): 919–32. http://dx.doi.org/10.1051/0004-6361:20053571.

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4

Schulz, H. y C. Henkel. "Rotation and outflow in the central kiloparsec of the water-megamaser galaxies IC 2560, NGC 1386, NGC 1052, and Mrk 1210". Astronomy & Astrophysics 400, n.º 1 (24 de febrero de 2003): 41–62. http://dx.doi.org/10.1051/0004-6361:20021735.

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5

Rodríguez-Ardila, A., M. A. Prieto, X. Mazzalay, J. A. Fernández-Ontiveros, R. Luque y F. Müller-Sánchez. "Powerful outflows in the central parsecs of the low-luminosity active galactic nucleus NGC 1386". Monthly Notices of the Royal Astronomical Society 470, n.º 3 (7 de junio de 2017): 2845–60. http://dx.doi.org/10.1093/mnras/stx1401.

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6

Weaver, K. A., A. S. Wilson y J. A. Baldwin. "Kinematics and ionization of extended gas in active galaxies. VI - The Seyfert 2 galaxy NGC 1386". Astrophysical Journal 366 (enero de 1991): 50. http://dx.doi.org/10.1086/169539.

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7

Saade, M. Lynne, Murray Brightman, Daniel Stern, Matthew A. Malkan y Javier A. García. "NuSTAR Observations of AGNs with Low Observed X-Ray to [O iii] Luminosity Ratios: Heavily Obscured AGNs or Turned-off AGNs?" Astrophysical Journal 936, n.º 2 (1 de septiembre de 2022): 162. http://dx.doi.org/10.3847/1538-4357/ac88cf.

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Abstract Type 2 active galactic nuclei (AGNs) show signatures of accretion onto a supermassive black hole through strong, high-ionization, narrow emission lines extended on scales of hundreds to thousands of parsecs, but they lack the broad emission lines from close in to the black hole that characterize type 1 AGNs. The lack of broad emission could indicate obscuration of the innermost nuclear regions, or could indicate that the black hole is no longer strongly accreting. Since high-energy X-rays can penetrate thick obscuring columns, they have the power to distinguish these two scenarios. We present high-energy NuSTAR observations of nine Seyfert 2 AGNs from the Infrared Astronomical Satellite 12 μm survey, supplemented with low-energy X-ray observations from Chandra, XMM-Newton, and Swift. The galaxies were selected to have anomalously low observed 2–10 keV luminosities compared to their [O iii] optical luminosities, a traditional diagnostic of heavily obscured AGNs, reaching into the Compton-thick regime for the highest hydrogen column densities (N H > 1.5 × 1024 cm−2). Based on updated [O iii] luminosities and intrinsic X-ray luminosities based on physical modeling of the hard X-ray spectra, we find that one galaxy was misclassified as type 2 (NGC 5005) and most of the remaining AGNs are obscured, including three confirmed as Compton thick (IC 3639, NGC 1386, and NGC 3982). One galaxy, NGC 3627, appears to have recently deactivated. Compared to the original sample that the nine AGNs were selected from, this is a rate of approximately 1%. We also find a new X-ray changing-look AGN in NGC 6890.

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8

Lena, D., A. Robinson, T. Storchi-Bergman, A. Schnorr-Müller, T. Seelig, R. A. Riffel, N. M. Nagar, G. S. Couto y L. Shadler. "THE COMPLEX GAS KINEMATICS IN THE NUCLEUS OF THE SEYFERT 2 GALAXY NGC 1386: ROTATION, OUTFLOWS, AND INFLOWS". Astrophysical Journal 806, n.º 1 (9 de junio de 2015): 84. http://dx.doi.org/10.1088/0004-637x/806/1/84.

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9

Strohmayer, Tod E. y Richard F. Mushotzky. "EVIDENCE FOR AN INTERMEDIATE-MASS BLACK HOLE IN NGC 5408 X-1". Astrophysical Journal 703, n.º 2 (9 de septiembre de 2009): 1386–93. http://dx.doi.org/10.1088/0004-637x/703/2/1386.

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10

Violat-Bordonau, Francisco. "L199, A NEW VARIABLE STAR IN M13". Open European Journal on Variable Stars, n.º 213 (abril de 2021): 1–10. http://dx.doi.org/10.5817/oejv2021-0213.

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During a routine study of the variable stars of Messier 13 (NGC 6205 = Cl 1639+365) we have discovered the variability of L199 (TYC 2588-1386-2), a red giant star member of the cluster: using the photometric data –in V band– obtained in the 2019 and 2020 campaigns we have verified its variability. Data from the Zwicky Transient Facility (ZTF) and Deras et al. (2019) were utilized to determine its type of variability and period estimation: our data suggest that it is a semiregular red giant, similar to the other variables of this type of the cluster, whose cycles of photometric variation are not identical; we derived a period of ~27 days (although without a regular periodicity) and an amplitude smaller: 0.08 ± 0.03 magnitudes in V band although they may be somewhat larger or smaller. With this discovery the cluster now has 63 variable stars.

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11

Venturi, G., G. Cresci, A. Marconi, M. Mingozzi, E. Nardini, S. Carniani, F. Mannucci et al. "MAGNUM survey: Compact jets causing large turmoil in galaxies". Astronomy & Astrophysics 648 (abril de 2021): A17. http://dx.doi.org/10.1051/0004-6361/202039869.

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Context. Outflows accelerated by active galactic nuclei (AGN) are commonly observed in the form of coherent, mildly collimated high-velocity gas directed along the AGN ionisation cones and kinetically powerful (≳1044 − 45 erg s−1) jets. Recent works found that outflows can also be accelerated by low-power (≲1044 erg s−1) jets, and the most recent cosmological simulations indicate that these are the dominant source of feedback on sub-kiloparsec scales, but little is known about their effect on the galaxy host. Aims. We study the relation between radio jets and the distribution and kinematics of the ionised gas in IC 5063, NGC 5643, NGC 1068, and NGC 1386 as part of our survey of nearby Seyfert galaxies called Measuring Active Galactic Nuclei Under MUSE Microscope (MAGNUM). All these objects host a small-scale (≲1 kpc) low-power (≲1044 erg s−1) radio jet that has small inclinations (≲45°) with respect to the galaxy disc. Methods. We employed seeing-limited optical integral field spectroscopic observations from the Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope to obtain flux, kinematic, and excitation maps of the extended ionised gas. We compared these maps with archival radio images and in one case, with Chandra X-ray observations. Results. We detect a strong (up to ≳800–1000 km s−1) and extended (≳1 kpc) emission-line velocity spread perpendicular to the direction of the AGN ionisation cones and jets in all four targets. The gas excitation in this region of line-width enhancement is entirely compatible with shock ionisation. These broad and symmetric line profiles are not associated with a single coherent velocity of the gas. A ‘classical’ outflow component with net blueshifted and redshifted motions is also present, but is directed along the ionisation cones and jets. Conclusions. We interpret the observed phenomenon as due to the action of the jets perturbing the gas in the galaxy disc. These intense and extended velocity spreads perpendicular to AGN jets and cones are indeed currently only observed in galaxies hosting a low-power jet whose inclination is sufficiently low with respect to the galaxy disc to impact on and strongly affect its material. In line with cosmological simulations, our results demonstrate that low-power jets are indeed capable of affecting the host galaxy.

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12

Cantiello, Michele, Aku Venhola, Aniello Grado, Maurizio Paolillo, Raffaele D’Abrusco, Gabriella Raimondo, Massimo Quintini et al. "The Fornax Deep Survey with VST". Astronomy & Astrophysics 639 (julio de 2020): A136. http://dx.doi.org/10.1051/0004-6361/202038137.

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Context. A possible pathway for understanding the events and the mechanisms involved in galaxy formation and evolution is an in-depth investigation of the galactic and inter-galactic fossil sub-structures with long dynamical timescales: stars in the field and in stellar clusters. Aims. This paper continues the Fornax Deep Survey (FDS) series. Following previous studies dedicated to extended Fornax cluster members, we present the catalogs of compact stellar systems in the Fornax cluster, as well as extended background sources and point-like sources. Methods. We derived ugri photometry of ∼1.7 million sources over the ∼21 square degree area of FDS centered on the bright central galaxy NGC 1399. For a wider area, of ∼27 square degrees extending in the direction of NGC 1316, we provided gri photometry for ∼3.1 million sources. To improve the morphological characterization of sources, we generated multi-band image stacks by coadding the best-seeing gri-band single exposures with a cut at full width at half maximum (FWHM) ≤ 0.″9. We used the multi-band stacks as master detection frames, with a FWHM improved by ∼15% and a FWHM variability from field to field reduced by a factor of ∼2.5 compared to the pass-band with the best FWHM, namely the r-band. The identification of compact sources, in particular, globular clusters (GC), was obtained from a combination of photometric (e.g., colors, magnitudes) and morphometric (e.g., concentration index, elongation, effective radius) selection criteria, also taking as reference the properties of sources with well-defined classifications from spectroscopic or high-resolution imaging data. Results. Using the FDS catalogs, we present a preliminary analysis of GC distributions in the Fornax area. The study confirms and extends further previous results that were limited to a smaller survey area. We observed the inter-galactic population of GCs, a population of mainly blue GCs centered on NGC 1399, extending over ∼0.9 Mpc, with an ellipticity ϵ ∼ 0.65 and a small tilt in the direction of NGC 1336. Several sub-structures extend over ∼0.5 Mpc along various directions. Two of these structures do not cross any bright galaxy; one of them appears to be connected to NGC 1404, a bright galaxy close to the cluster core and particularly poor in GCs. Using the gri catalogs, we analyze the GC distribution over the extended FDS area and do not find any obvious GC sub-structure bridging the two brightest cluster galaxies, namely, NGC 1316 and NGC 1399. Although NGC 1316 is more than twice as bright of NGC 1399 in optical bands, using gri data, we estimate a GC population that is richer by a factor of ∼3−4 around NGC 1399, as compared to NGC 1316, out to galactocentric distances of ∼40′ or ∼230 kpc.

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13

Gómez, Matías, Tom Richtler, Leopoldo Infante y Georg Drenkhahn. "The Globular Cluster System of NGC 1316". Symposium - International Astronomical Union 207 (2002): 321–23. http://dx.doi.org/10.1017/s0074180900223954.

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We have studied the Globular Cluster System of the merger galaxy NGC 1316 in Fornax, using CCD BV I photometry. Dividing the sample into red (presumably metal-rich) and blue (metal-poor) subpopulations at B - I = 1.75, we find that they follow strikingly different angular distributions. The red clusters show a strong correlation with the galaxy elongation, but the blue ones are circularly distributed. An astonishingly low specific frequency for NGC 1316 of only SN = 0.9±0.2 is derived, which confirms with a larger field a previous finding by Grillmair et al. (1999). Assuming a “normal” SN of ∼ 4 for early-type galaxies, we use stellar population synthesis models to estimate the merger age to about 2 Gyr, if an intermediate-age population were to explain the low SN we observe. By fitting t5 functions to the Globular Cluster Luminosity Function (GCLF), we derive the following turnover magnitudes: and . They support that NGC 1316, in spite of its outlying location, is at the same distance as the core of the Fornax cluster.

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14

Senarath, Madhooshi R., M. J. I. Brown, Michelle E. Cluver, Thomas H. Jarrett y Nicholas P. Ross. "The Nearby “Changing Look” Seyfert NGC 1346". Research Notes of the AAS 3, n.º 4 (17 de abril de 2019): 62. http://dx.doi.org/10.3847/2515-5172/ab191d.

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15

Richtler, T., M. Hilker, B. Kumar, L. P. Bassino, M. Gómez y B. Dirsch. "The globular cluster system of NGC 1316". Astronomy & Astrophysics 569 (septiembre de 2014): A41. http://dx.doi.org/10.1051/0004-6361/201423525.

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16

Richtler, T., L. P. Bassino, B. Dirsch y B. Kumar. "The globular cluster system of NGC 1316". Astronomy & Astrophysics 543 (julio de 2012): A131. http://dx.doi.org/10.1051/0004-6361/201118589.

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17

Richtler, T., B. Kumar, L. P. Bassino, B. Dirsch y A. J. Romanowsky. "The globular cluster system of NGC 1316". Astronomy & Astrophysics 543 (julio de 2012): L7. http://dx.doi.org/10.1051/0004-6361/201219075.

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18

Richtler, T., B. Husemann, M. Hilker, T. H. Puzia, F. Bresolin y M. Gómez. "The globular cluster system of NGC 1316". Astronomy & Astrophysics 601 (24 de abril de 2017): A28. http://dx.doi.org/10.1051/0004-6361/201630227.

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19

Franco, Jose, J. Antonio Garcia‐Barreto y Eduardo de la Fuente. "Decreasing Density Gradients in Circumnuclear HiiRegions of Barred Galaxies NGC 1022, NGC 1326, and NGC 4314". Astrophysical Journal 544, n.º 1 (20 de noviembre de 2000): 277–82. http://dx.doi.org/10.1086/317189.

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20

Serra, P., F. M. Maccagni, D. Kleiner, W. J. G. de Blok, J. H. van Gorkom, B. Hugo, E. Iodice et al. "Neutral hydrogen gas within and around NGC 1316". Astronomy & Astrophysics 628 (agosto de 2019): A122. http://dx.doi.org/10.1051/0004-6361/201936114.

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We present MeerKAT observations of neutral hydrogen gas (H I) in the nearby merger remnant NGC 1316 (Fornax A), the brightest member of a galaxy group which is falling into the Fornax cluster. We find H I on a variety of scales, from the galaxy centre to its large-scale environment. For the first time we detect H I at large radii (70–150 kpc in projection), mostly distributed on two long tails associated with the galaxy. Gas in the tails dominates the H I mass of NGC 1316: 7 × 108 M⊙– 14 times more than in previous observations. The total H I mass is comparable to the amount of neutral gas found inside the stellar body, mostly in molecular form. The H I tails are associated with faint optical tidal features thought to be the remnant of a galaxy merger occurred a few billion years ago. They demonstrate that the merger was gas-rich. During the merger, tidal forces pulled some gas and stars out to large radii, where we now detect them in the form of optical tails and, thanks to our new data, H I tails; while torques caused the remaining gas to flow towards the centre of the remnant, where it was converted into molecular gas and fuelled the starburst revealed by the galaxy’s stellar populations. Several of the observed properties of NGC 1316 can be reproduced by a ∼10:1 merger between a dominant, gas-poor early-type galaxy and a smaller, gas-rich spiral occurred 1–3 Gyr ago, likely followed by subsequent accretion of satellite galaxies.

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21

Napolitano, N. R., M. Gatto, C. Spiniello, M. Cantiello, M. Hilker, M. Arnaboldi, C. Tortora et al. "The Fornax Cluster VLT Spectroscopic Survey". Astronomy & Astrophysics 657 (enero de 2022): A94. http://dx.doi.org/10.1051/0004-6361/202141872.

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Context. Substructures in stellar haloes are a strong prediction of galaxy formation models in ΛCDM. Cold streams such as those from small satellite galaxies are extremely difficult to detect and kinematically characterize. The COld STream finder Algorithm (COSTA) is a novel algorithm able to find streams in the phase space of planetary nebulae (PNe) and globular cluster (GC) populations. COSTA isolates groups of (N) particles with small velocity dispersion (between 10 km s−1 and ∼120 km s−1) using an iterative (n) sigma-clipping over a defined number of (k) neighbor particles. Aims. We applied COSTA to a catalog of PNe and GCs from the Fornax Cluster VLT Spectroscopic Survey (FVSS) within ∼200 kpc from the cluster core in order to detect cold substructures and characterize their kinematics (mean velocity and velocity dispersion). Methods. We selected more than 2000 PNe and GCs from the FVSS catalogs and adopted a series of optimized setups of the COSTA parameters based on Montecarlo simulations of the PN and GC populations to search for realistic stream candidates. We find 13 cold substructures with velocity dispersion ranging from ∼20 to ∼100 km s−1, which are likely associated either to large galaxies or to ultra-compact dwarf (UCD) galaxies in the Fornax core. Results. The luminosities of these streams show a clear correlation with internal velocity dispersion, and their surface brightness correlates with their size and distance from the cluster center, which is compatible with the dissipative processes producing them. However, we cannot exclude that some of these substructures formed by violent relaxation of massive satellites that finally merged into the central galaxy. Among these substructures we have: (1) a stream connecting NGC 1387 to the central galaxy, NGC 1399, previously reported in the literature; (2) a new giant stream produced by the interaction of NGC 1382 with NGC 1380 and (possibly) NGC 1381; (3) a series of streams kinematically connected to nearby UCDs; and (4) clumps of tracers with no clear kinematical association to close cluster members. Conclusions. We show evidence for a variety of cold substructures predicted in simulations. Most of the streams are kinematically connected to UCDs, supporting the scenario that they can be remnants of disrupted dwarf systems. However, we also show the presence of long coherent substructures connecting cluster members and isolated clumps of tracers possibly left behind by their parent systems before these merged into the central galaxy. Unfortunately, the estimated low-surface brightness of these streams does not allow us to find their signatures in the current imaging data and deeper observations are needed to confirm them.

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22

Sesto, Leandro, Favio Faifer, Juan Forte y Analía Castelli. "Deep MOS Spectroscopy of NGC 1316 Globular Clusters". Galaxies 5, n.º 3 (15 de agosto de 2017): 39. http://dx.doi.org/10.3390/galaxies5030039.

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23

Fazeli, Nastaran, Gerold Busch, Andreas Eckart, Françoise Combes, Persis Misquitta y Christian Straubmeier. "Central kiloparsec of NGC 1326 observed with SINFONI". Astronomy & Astrophysics 638 (junio de 2020): A53. http://dx.doi.org/10.1051/0004-6361/201936451.

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Gas inflow processes in the vicinity of galactic nuclei play a crucial role in galaxy evolution and supermassive black hole growth. Exploring the central kiloparsec of galaxies is essential to shed more light on this subject. We present near-infrared H- and K-band results of the nuclear region of the nearby galaxy NGC 1326, observed with the integral-field spectrograph SINFONI mounted on the Very Large Telescope. The field of view covers 9″ × 9″ (650 × 650 pc2). Our work is concentrated on excitation conditions, morphology, and stellar content. The nucleus of NGC 1326 was classified as a LINER, however in our data we observed an absence of ionised gas emission in the central r ∼ 3″. We studied the morphology by analysing the distribution of ionised and molecular gas, and thereby detected an elliptically shaped, circum-nuclear star-forming ring at a mean radius of 300 pc. We estimate the starburst regions in the ring to be young with dominating ages of < 10 Myr. The molecular gas distribution also reveals an elongated east to west central structure about 3″ in radius, where gas is excited by slow or mild shock mechanisms. We calculate the ionised gas mass of 8 × 105 M⊙ completely concentrated in the nuclear ring and the warm molecular gas mass of 187 M⊙, from which half is concentrated in the ring and the other half in the elongated central structure. The stellar velocity fields show pure rotation in the plane of the galaxy. The gas velocity fields show similar rotation in the ring, but in the central elongated H2 structure they show much higher amplitudes and indications of further deviation from the stellar rotation in the central 1″ aperture. We suggest that the central 6″ elongated H2 structure might be a fast-rotating central disc. The CO(3–2) emission observations with the Atacama Large Millimeter/submillimeter Array reveal a central 1″ torus. In the central 1″ of the H2 velocity field and residual maps, we find indications for a further decoupled structure closer to a nuclear disc, which could be identified with the torus surrounding the supermassive black hole.

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24

Kim, Dong‐Woo y G. Fabbiano. "ChandraX‐Ray Observations of NGC 1316 (Fornax A)". Astrophysical Journal 586, n.º 2 (abril de 2003): 826–49. http://dx.doi.org/10.1086/367930.

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25

Kabasares, Kyle M., Aaron J. Barth, David A. Buote, Benjamin D. Boizelle, Jonelle L. Walsh, Andrew J. Baker, Jeremy Darling, Luis C. Ho y Jonathan Cohn. "Black Hole Mass Measurements of Early-type Galaxies NGC 1380 and NGC 6861 through ALMA and HST Observations and Gas-dynamical Modeling*". Astrophysical Journal 934, n.º 2 (1 de agosto de 2022): 162. http://dx.doi.org/10.3847/1538-4357/ac7a38.

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Abstract We present Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 2 observations of CO(2–1) emission from the circumnuclear disks in two early-type galaxies, NGC 1380 and NGC 6861. The disk in each galaxy is highly inclined (i ∼ 75°), and the projected velocities of the molecular gas near the galaxy centers are ∼300 km s−1 in NGC 1380 and ∼500 km s−1 in NGC 6861. We fit thin disk dynamical models to the ALMA data cubes to constrain the masses of the central black holes (BHs). We created host galaxy models using Hubble Space Telescope images for the extended stellar mass distributions and incorporated a range of plausible central dust extinction values. For NGC 1380, our best-fit model yields M BH = 1.47 × 108 M ⊙ with a ∼40% uncertainty. For NGC 6861, the lack of dynamical tracers within the BH’s sphere of influence due to a central hole in the gas distribution precludes a precise measurement of M BH. However, our model fits require a value for M BH in the range of (1–3) × 109 M ⊙ in NGC 6861 to reproduce the observations. The BH masses are generally consistent with predictions from local BH–host galaxy scaling relations. Systematic uncertainties associated with dust extinction of the host galaxy light and choice of host galaxy mass model dominate the error budget of both measurements. Despite these limitations, the measurements demonstrate ALMA’s ability to provide constraints on BH masses in cases where the BH’s projected radius of influence is marginally resolved or the gas distribution has a central hole.

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26

McNeil-Moylan, E. K., K. C. Freeman, M. Arnaboldi y O. E. Gerhard. "Planetary nebula kinematics in NGC 1316: a young Sombrero". Astronomy & Astrophysics 539 (17 de febrero de 2012): A11. http://dx.doi.org/10.1051/0004-6361/201117875.

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27

Gómez, M., T. Richtler, L. Infante y G. Drenkhahn. "The globular cluster system of NGC 1316 (Fornax A)". Astronomy & Astrophysics 371, n.º 3 (junio de 2001): 875–89. http://dx.doi.org/10.1051/0004-6361:20010457.

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28

Iyomoto, Naoko, Kazuo Makishima, Makoto Tashiro, Susumu Inoue, Hidehiro Kaneda, Yukari Matsumoto y Tsunefumi Mizuno. "The Declined Activity in the Nucleus of NGC 1316". Astrophysical Journal 503, n.º 1 (10 de agosto de 1998): L31—L34. http://dx.doi.org/10.1086/311518.

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29

Richtler, T., M. Hilker y E. Iodice. "Dust and gas in the central region of NGC 1316 (Fornax A)". Astronomy & Astrophysics 643 (noviembre de 2020): A120. http://dx.doi.org/10.1051/0004-6361/202038150.

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Context. The early-type galaxy NGC 1316, associated with the radio source Fornax A, hosts about 107 M⊙ of dust within a central radius of 5 kpc. These prominent dust structures are believed to have an external origin, which is also a popular interpretation for other dusty early-type galaxies. Moreover, it has been long known that ionised gas is present in NGC 1316, but to date there has been a lack of detailed investigation. Aims. Our aim is to understand the nature of ionised gas and dust in NGC 1316 and to offer an interpretation for the origin of the dust. Methods. We use archival Hubble Space Telescope/Advanced Camera for Surveys data to construct colour maps that delineate the dust pattern in detail, and we compare these data with maps constructed with data from the Multi Unit Spectroscopic Explorer (MUSE) instrument of the Very Large Telescope at the European Southern Observatory. Twelve MUSE pointings in wide field mode form a mosaic of the central 3.3 × 2.4 arcmin2. We use the tool PyParadise to fit the stellar population. We use the residual emission lines and the residual interstellar absorption NaI D-lines, and we measure line strengths, the velocity field, and the velocity dispersion field. Results. The emission lines resemble low-ionisation nuclear emission-line region lines, with [NII] being the strongest line everywhere. Ionising sources are plausibly the post-asymptotic giant branch stars of the old or intermediate-age stellar population. There is a striking match between the dust structures, ionised gas, and atomic gas distributions, the last of which is manifested by interstellar absorption residuals of the stellar NaI D-lines. In the dust-free regions, the interstellar NaI D-lines appear in emission, which is indicative of a galactic wind. The velocity field of the ionised gas (and thus of the dust) is characterised by small-scale turbulent movements that indicate short lifetimes. At the very centre, a bipolar velocity field of the ionised gas is observed, which we interpret as an outflow. The low-velocity part is associated with dust. We identify a strongly inclined gaseous dusty disc along the major axis of NGC 1316. A straight beam of ionised gas with a length of about 4 kpc emanates from the centre. Conclusions. The dust in NGC 1316 has different origins. Our findings are strongly suggestive of a dusty outflow that is curved along the line-of-sight. Nuclear outflows may be important dust-producing machines in galaxies. Another dusty gaseous component forms a disc that we identify as the predecessor of a central dust lane.

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30

Goudfrooij, Paul. "3-Gyr-old Globular Clusters in the Merger Remnant NGC 1316: Implications for the Fate of Globular Clusters Formed During Gas-rich Galaxy Mergers". Symposium - International Astronomical Union 207 (2002): 245–50. http://dx.doi.org/10.1017/s0074180900223802.

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The giant early-type merger remnant galaxy NGC 1316 is an ideal probe for studying the long-term effects of a major merger on its globular cluster (GC) system, given its spectroscopically derived merger age of ∼3 Gyr which we reported in a recent paper. Here we report several pieces of photometric evidence showing that the second-generation GCs in NGC 1316 are at an evolutionary phase in between that of luminous GCs found in younger merger remnants such as (e.g.) NGC 7252 and that of ‘red’ GCs found in ‘normal, old’ ellipticals. The observation that massive, second-generation GCs formed during major mergers can survive for at least 3 Gyr provides strong evidence that these clusters can have ‘normal’ mass functions including low-mass stars, and hence that they can survive to reach ‘old age’ similar to those of ‘normal’ ellipticals.

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31

Sesto, Leandro A., Favio R. Faifer y Juan C. Forte. "The complex star cluster system of NGC 1316 (Fornax A)". Monthly Notices of the Royal Astronomical Society 461, n.º 4 (7 de julio de 2016): 4260–75. http://dx.doi.org/10.1093/mnras/stw1627.

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32

J. Grillmair, Carl, Jon Holtzman y Rebecca Elson. "Resolving Globular Clusters in the Fornax Cluster and Beyond". Symposium - International Astronomical Union 207 (2002): 327–29. http://dx.doi.org/10.1017/s0074180900223978.

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We describe an ongoing program to measure structural parameters for globular clusters with a range of ages in early-type galaxies. Using deep, optimally-dithered HST WFPC2 observations of NGC 3597, NGC 1316, and NGC 1399, we apply a χ2 minimization method to the determination of cluster sizes. The goals include studying the structure spectrum of stellar clusters at birth, and determining the rate at which tidal and evaporative destruction mechanisms operate to alter luminosity functions and specific frequencies to what we see in ellipticals today.

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33

Shaya, E. J., D. M. Dowling, D. G. Currie, S. M. Faber, E. A. Ajhar, T. R. Lauer, E. J. Groth, C. J. Grillmair, R. Lynd y E. J. ,. Jr O'Neil. "Hubble Space Telescope Planetary Camera Images of NGC 1316 (Fornax A)". Astronomical Journal 111 (junio de 1996): 2212. http://dx.doi.org/10.1086/117955.

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34

Cantiello, M., A. Grado, J. P. Blakeslee, G. Raimondo, G. Di Rico, L. Limatola, E. Brocato, M. Della Valle y R. Gilmozzi. "The distance to NGC 1316 (Fornax A): yet another curious case". Astronomy & Astrophysics 552 (abril de 2013): A106. http://dx.doi.org/10.1051/0004-6361/201220756.

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35

Allak, S., A. Akyuz, N. Aksaker, M. Ozdogan Ela, S. Avdan y F. Soydugan. "Identification of a new ultraluminous X-ray source in NGC 1316". Monthly Notices of the Royal Astronomical Society 499, n.º 4 (4 de noviembre de 2020): 5682–89. http://dx.doi.org/10.1093/mnras/staa3073.

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ABSTRACT In this study, we report identification of a new ultraluminous X-ray source (ULX) named as X-7 in NGC 1316, with an unabsorbed luminosity of 2.1 × 1039 erg s−1 using the two recent Chandra archival observations. The X-7 was detected in the Chandra 2001 observation and was included in the source list of the NGC 1316 as CXOUJ032240.8−371224 with a luminosity of 5.7 × 1038 erg s−1. Present luminosity implies a luminosity increase of a factor of ∼4. The best-fitting spectral model parameters indicate that X-7 has a relatively hot disc and hard spectra. If explained by a disc blackbody model, the mass of compact object is estimated as ∼8 M⊙ which is in the range of a stellar-mass black hole. The X-7 shows a relatively long-term count rate variability while no short-term variability is observed. We also identified a unique optical candidate within 0.22 arcsec error circle at 95 per cent confidence level for X-7 using the archival HST/ACS (Hubble Space Telescope/Advanced Camera for Surveys) and HST/WFC3 (The Wide Field Camera 3) data. Absolute magnitude (MV) of this candidate is −7.8 mag. Its spectral energy distribution is adequately fitted a blackbody model with a temperature of 3100 K indicating an M type supergiant, assuming the donor star dominates the optical emission. In addition, we identified a transient ULX candidate (XT-1) located 6 arcsec away from X-7 has a (high) luminosity of ∼1039 erg s−1 with no visible optical candidate.

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36

Kim, D. W., G. Fabbiano y G. Mackie. "ROSATX−Ray Observations of the Radio Galaxy NGC 1316 (Fornax A)". Astrophysical Journal 497, n.º 2 (20 de abril de 1998): 699–712. http://dx.doi.org/10.1086/305476.

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37

Duah Asabere, B., C. Horellou, T. H. Jarrett y H. Winkler. "Mid-infrared dust in two nearby radio galaxies, NGC 1316 (Fornax A) and NGC 612 (PKS 0131-36)". Astronomy & Astrophysics 592 (5 de julio de 2016): A20. http://dx.doi.org/10.1051/0004-6361/201528047.

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38

Dage, Kristen C., Arunav Kundu, Erica Thygesen, Arash Bahramian, Daryl Haggard, Jimmy A. Irwin, Thomas J. Maccarone et al. "Three ultraluminous X-ray sources hosted by globular clusters in NGC 1316". Monthly Notices of the Royal Astronomical Society 504, n.º 1 (5 de abril de 2021): 1545–54. http://dx.doi.org/10.1093/mnras/stab943.

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ABSTRACT We have identified three ultraluminous X-ray sources (ULXs) hosted by globular clusters (GCs) within NGC 1316’s stellar system. These discoveries bring the total number of known ULXs in GCs up to 20. We find that the X-ray spectra of the three new sources do not deviate from the established pattern of spectral behaviour of the other known GC ULXs. The consistency of the X-ray spectral behaviour for these sources points to multiple paths of formation and evolution mechanisms for these rare and unique sources. Using the now larger sample of GC ULXs, we compare the optical properties of the entire known population of GC ULXs to other GCs across five galaxies and find that the properties of clusters that host ULXs are quite different from the typical clusters. Lastly, any trend of GC ULXs being preferentially hosted by metal-rich clusters is not strongly significant in this sample.

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39

Schlegel, Eric M., Robert Petre y Michael Loewenstein. "[ITAL]ROSAT[/ITAL] Observations of X-Ray–faint S0 Galaxies: NGC 1380". Astronomical Journal 115, n.º 2 (febrero de 1998): 525–34. http://dx.doi.org/10.1086/300217.

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40

Maoz, Dan y Filippo Mannucci. "A search for the progenitors of two TypeIa Supernovae in NGC 1316". Monthly Notices of the Royal Astronomical Society 388, n.º 1 (21 de julio de 2008): 421–28. http://dx.doi.org/10.1111/j.1365-2966.2008.13403.x.

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41

Konami, S., K. Matsushita, K. Sato, R. Nagino, N. Isobe, M. S. Tashiro, H. Seta, K. Matsuta, T. Tamagawa y K. Makishima. "Suzaku observation of the metallicity in the interstellar medium of NGC 1316". Proceedings of the International Astronomical Union 5, H15 (noviembre de 2009): 286. http://dx.doi.org/10.1017/s1743921310009294.

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Metal abundances of the hot X-ray emitting interstellar medium (ISM) include important information to understand the history of star formation and evolution of galaxies. The metals are mainly synthesized by Type Ia (SNe Ia) and stellar mass loss in elliptical galaxies. The productions of stellar mass loss reflect stellar metallicity. SNe Ia mainly product Fe. Therefore, the abundance pattern of ISM can play key role to investigate the metal enrichment history.

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42

Buta, R. "Star Clusters in Galactic Resonance Rings". Symposium - International Astronomical Union 207 (2002): 447–49. http://dx.doi.org/10.1017/s0074180900224169.

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Resonance rings are intriguing sites of organized star formation in some galaxies. The Hubble Space Telescope Wide Field and Planetary Camera 2 has been used to image several resonance rings at high resolution in order to study the star clusters in the rings. Here I summarize results on inner Lindblad resonance rings in ESO 565–11 and NGC 1326, and on an inner 4:1 resonance ring in the Seyfert 2 galaxy NGC 3081. The latter ring provides one of the strongest cases illustrating the connection between star formation and dynamics in disk galaxies.

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43

Fabbiano, G., C. Fassnacht y G. Trinchieri. "High resolution optical and UV observations of the centers of NGC 1316 and NGC 3998 with the Hubble Space Telescope". Astrophysical Journal 434 (octubre de 1994): 67. http://dx.doi.org/10.1086/174705.

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44

Mackie, G. y G. Fabbiano. "Evolution of Gas and Stars in the Merger Galaxy NGC 1316 (Fornax A)". Astronomical Journal 115, n.º 2 (febrero de 1998): 514–24. http://dx.doi.org/10.1086/300203.

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45

Bosma, A., R. M. Smith y K. J. Wellington. "Rotation and velocity dispersion in the stellar component of NGC 1316 (Fornax A)". Monthly Notices of the Royal Astronomical Society 212, n.º 2 (1 de enero de 1985): 301–7. http://dx.doi.org/10.1093/mnras/212.2.301.

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46

Mazzolini, Margaret y Rachel Webster. "Preliminary Radio Continuum Maps of Three Spiral Galaxies". Publications of the Astronomical Society of Australia 13, n.º 2 (mayo de 1996): 107–20. http://dx.doi.org/10.1017/s1323358000020646.

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AbstractThe Australia Telescope Compact Array has been used in two 6 km configurations to make 12 hour observations of the radio continuum structure of three spiral galaxies at 1380 MHz and 2378 MHz. Radio maps of NGC 1792, 6300 and 1097 are presented here, as part of a survey to find examples of anomalous radio structures in spiral galaxies.

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47

Jacoby, G. H., J. Morse y L. Fullton. "The Planetary Nebulae in NGC 6441 and Pal 6". Symposium - International Astronomical Union 180 (1997): 243. http://dx.doi.org/10.1017/s0074180900130621.

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Jacoby & Fullton (1994, BAAS, 26, 1384) searched 133 of the ∼ 150 Galactic globular clusters for Planetary Nebulae (PNe) using the on-band/off-band imaging technique at [O III] λ5007Å. We present preliminary abundances and central star properties for the 2 new PN identified in that survey (labeled JaFu 1 and JaFu 2 by Acker, Marcout, & Ochsenbein 1996).

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48

Smith, Russell J. "Discovering novae in early-type galaxies with MUSE: A chance find in NGC 1404, and 12 more candidates from an archival search". Monthly Notices of the Royal Astronomical Society: Letters 494, n.º 1 (7 de febrero de 2020): L1—L5. http://dx.doi.org/10.1093/mnrasl/slaa023.

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ABSTRACT I report the discovery of a transient broad-Hα point source in the outskirts of the giant elliptical galaxy NGC 1404, discovered in archival observations taken with the Multi-Unit Spectroscopic Explorer (MUSE) integral field spectrograph. The Hα line width of 1950 km s−1 full width at half-maximum, and luminosity of (4.1 ± 0.1) × 1036 erg s−1, are consistent with a nova outburst, and the source is not visible in MUSE data obtained 9 months later. A transient soft X-ray source was detected at the same position (within <1 arcsec), 14 yr before the Hα transient. If the X-ray and Hα emission are from the same object, the source may be a short-time-scale recurrent nova with a massive white dwarf accretor, and hence a possible Type-Ia supernova progenitor. Selecting broad-Hα point sources in MUSE archival observations for a set of nearby early-type galaxies, I discovered 12 more nova candidates with similar properties to the NGC 1404 source, including five in NGC 1380 and four in NGC 4365. Multi-epoch data are available for four of these twelve sources; all four are confirmed to be transient on ∼1 yr time-scales, supporting their identification as novae.

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49

Buta, R., Patrick M. Treuthardt, G. G. Byrd y D. A. Crocker. "Circumnuclear Star Formation in the Early-Type Resonance Ring Barred Spiral Galaxy NGC 1326". Astronomical Journal 120, n.º 3 (septiembre de 2000): 1289–305. http://dx.doi.org/10.1086/301531.

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50

Stritzinger, Maximilian, Christopher R. Burns, Mark M. Phillips, Gastón Folatelli, Kevin Krisciunas, ShiAnne Kattner, Sven E. Persson et al. "THE DISTANCE TO NGC 1316 (FORNAX A) FROM OBSERVATIONS OF FOUR TYPE Ia SUPERNOVAE". Astronomical Journal 140, n.º 6 (11 de noviembre de 2010): 2036–51. http://dx.doi.org/10.1088/0004-6256/140/6/2036.

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