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Similar to Figure 1 but for the AGN fraction in the control sample as a function of redshift and stellar mass. The model in the inset is given in Equation (13). The contours show the distribution of the control sample at dN ctrl =(8, 46, 84, 122) per cell.
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We have identified 105 galaxy pairs at z ~ 0.04 with the MaNGA integral-field spectroscopic data. The pairs have projected separations between 1 kpc and 30 kpc, and are selected to have radial velocity offsets less than 600 km/s and stellar mass ratio between 0.1 and 1. The pair fraction increases with both the physical size of the integral-field u...
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... does not depend on the size of the IFU as the pair fraction does. In Figure 3, we show the AGN fraction in the control sample as a function of the two parameters. We define the 2D AGN fraction as ...
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... simple calculation suggests that there could be a significant population of correlated starforming galaxies and RGs. But a more rigorous investigation requires quantifying the stellar mass dependence of starforming and retired fractions in the control sample (similar to Figure 3 and Equation (13) for AGNs) and utilizing the 1/V max weights described in Section 2.1 to compare the observed and expected volume densities. In the next subsection, we will carry out such an investigation on correlated AGNs. ...
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... it could also be due to the selection bias of the pair sample. Recall that the pair sample is biased to high stellar mass and large IFU size (and consequently, to high redshift) when compared to the parent sample (Figure 1), and the AGN fraction varies with stellar mass and redshift (Figure 3 and Equation (13)). On the other hand, the number of binary AGNs (14/105 or 13%) is significantly higher than expected from random pairing: one would expect only ∼6 binaries (=105 × 22% × 26%) even given the high AGN fractions in pairs. ...
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... These ENLRs have a wide range of physical sizes, from a few kpc (e.g. Fu et al. 2012Fu et al. , 2018 and -in some cases -extending up to tens of kpc from the central AGN (e.g. Greene et al. 2011Greene et al. , 2012Stockton et al. 2006;Hainline et al. 2016), and they have been identified in candidate (Greene et al. , 2012Fu et al. 2012Fu et al. , 2018, ∼few kpc-scale) and confirmed (Fu et al. 2012;Hainline et al. 2016, ∼ 30 kpc-scale) dual AGN systems. ...
... Fu et al. 2012Fu et al. , 2018 and -in some cases -extending up to tens of kpc from the central AGN (e.g. Greene et al. 2011Greene et al. , 2012Stockton et al. 2006;Hainline et al. 2016), and they have been identified in candidate (Greene et al. , 2012Fu et al. 2012Fu et al. , 2018, ∼few kpc-scale) and confirmed (Fu et al. 2012;Hainline et al. 2016, ∼ 30 kpc-scale) dual AGN systems. Cross-ionization (Keel et al. 2019), where one AGN in a galaxy pair ionizes the gas in the companion galaxy, is a specific kind of ENLR and can mimic the presence of a dual or multi-AGN (Fu et al. 2012(Fu et al. , 2018 and is often invoked as an alternative hypothesis for the observation of multiple AGNlike emission line regions (e.g., Fu et al. 2012;Liu et al. 2018b;Fu et al. 2018;Liu et al. 2010bLiu et al. , 2011a. ...
... Greene et al. 2011Greene et al. , 2012Stockton et al. 2006;Hainline et al. 2016), and they have been identified in candidate (Greene et al. , 2012Fu et al. 2012Fu et al. , 2018, ∼few kpc-scale) and confirmed (Fu et al. 2012;Hainline et al. 2016, ∼ 30 kpc-scale) dual AGN systems. Cross-ionization (Keel et al. 2019), where one AGN in a galaxy pair ionizes the gas in the companion galaxy, is a specific kind of ENLR and can mimic the presence of a dual or multi-AGN (Fu et al. 2012(Fu et al. , 2018 and is often invoked as an alternative hypothesis for the observation of multiple AGNlike emission line regions (e.g., Fu et al. 2012;Liu et al. 2018b;Fu et al. 2018;Liu et al. 2010bLiu et al. , 2011a. To avoid erroneous bona fide dual AGN and multi-AGN classifications due to ENLRs and/or cross-ionization, we typically do not classify optically-selected multi-AGN candidates as confirmed systems (rank = 1) unless the multiwavelength evidence is overwhelming or the separations of the AGNs are sufficiently large enough that ENLRs are a lesser concern. ...
Galaxy mergers represent the most transformative and dramatic avenue for galaxy and supermassive black hole (SMBH) evolution. Multi-active galactic nuclei (multi-AGNs) are expected to ignite, grow, and evolve alongside the host galaxies, and these represent different evolutionary stages of the SMBHs over the merger sequence. However, no comprehensive census exists of observed multi-AGN systems. Here we present The Big Multi-AGN Catalog (The Big MAC), the first literature-complete catalog of all known (confirmed and candidate) multi-AGN systems, which includes dual AGNs (separations kpc), binary AGNs (gravitationally bound, pc), recoiling AGNs, and N-tuple AGNs (involving three or more AGNs), gleaned from hundreds of literature articles spanning the years 1970-2020. The Big MAC is the first archive to assemble all multi-AGN systems and candidates across all selection methods, redshifts, and galaxy mass ratios, and this catalog offers a solid foundation for archival and targeted multiwavelength follow-up investigations. In this work, we provide an overview of the creation of the multi-AGN literature library and the catalog itself, present definitions for different multi-AGN classes (including new definitions for dual AGNs derived from galaxy pairs in Illustris-TNG100), describe the general properties of the catalog as a function of redshift space and separation, and we provide a thorough examination of selection and confirmation method usage within the literature. We also discuss best practices for the multi-AGN literature, and we emphasize that a diverse, multiwavelength array of selection approaches is crucial for a complete understanding of multi-AGNs and - by extension - answering long-standing, open questions regarding the importance of AGNs and galaxy mergers.
... This difficulty arises from increased obscuration in late-stage mergers (e.g., Koss et al. 2016;Ricci et al. 2021;De Rosa et al. 2022), limitations in telescope spatial resolution (particularly at subkiloparsec scales), the scarcity of detected radio-bright dual systems (Burke-Spolaor 2011), and the limitations of optical selection using double-peaked narrow emission lines (prone to false positives; see Fu et al. 2011a). Existing observations of dual AGNs tentatively suggest that AGN triggering becomes more prevalent in advanced mergers with stellar bulge separations <10 kpc (e.g., Koss et al. 2010;Fu et al. 2018;Stemo et al. 2021), aligning with simulations of SMBH accretion and evolution in such mergers (e.g., Blecha et al. 2018). Therefore, studying nearby galaxies hosting dual AGNs separated at subkiloparsec scales is crucial for advancing our understanding of the late stages of galaxy mergers, the triggering and fueling of AGN activity, and the dynamics of SMBH pairs (Steinborn et al. 2016). ...
We report the serendipitous multiwavelength discovery of a candidate dual black hole system with a separation of ∼100 pc, in the gas-rich luminous infrared galaxy MCG-03-34-64 ( z = 0.016). Hubble Space Telescope/Advanced Camera for Surveys observations show three distinct optical centroids in the [O iii ] narrow-band and F814W images. Subsequent analysis of Chandra/ACIS data shows two spatially resolved peaks of equal intensity in the neutral Fe K α (6.2–6.6 keV) band, while high-resolution radio continuum observations with the Very Large Array at 8.46 GHz (3.6 cm band) show two spatially coincident radio peaks. Fast shocks as the ionizing source seem unlikely, given the energies required for the production of Fe K α . If confirmed, the separation of ∼100 pc would represent the closest dual active galactic nuclei reported to date with spatially resolved, multiwavelength observations.
... Despite a considerable amount of work on the search for galaxy pairs, the number of available samples for analysis is currently only a few thousand. Searching for more galaxy pair targets can provide researchers with a larger set of analysis samples, and help further understand the evolutionary processes of galaxies (Navasardyan et al. 2001;Focardi et al. 2006;Fu et al. 2018;Schreiber et al. 2018;Dai et al. 2021;Lin et al. 2022). ...
Galaxy pairs hold significant importance in understanding the evolution of galaxies, and the extensive search for a large sample of galaxy pairs is meaningful. In this article, we develop a deep learning-based approach for the search of galaxy pairs and conduct a comprehensive search on Sloan Digital Sky Survey (SDSS) images. In nine million photometric images, 17,965 physical galaxy pairs with spectral or photometric redshifts are detected. Four sets of results are provided, including physical pairs determined by two spectral redshifts, two photometric redshifts, one spectral redshift, and one photometric redshift, and visual irregular pairs that have no precise redshift information but can be inferred as physical galaxy pairs based on the morphological changes. Then their morphological and physical characteristics are explored, the redshifts of most targets are around 0.1, and as the redshift difference between two galaxies increases, the number of galaxy pairs gradually reduces. The distributions of star formation rate (SFR) are not the same for different morphologies of galaxy pairs, irregular pairs have higher SFR than the other three types, and statistics indicate that the SFR of galaxies depends on both nearby galaxies and internal properties. Color and stellar mass are also key properties of galaxies which can reflect the status of galaxy pairs. Compared to other surveys, a greater number of galaxy pair targets are detected, and this is also the first extensive detection of galaxy pairs in SDSS images using photometric redshifts. These galaxy pair samples can greatly aid in the study of galaxy evolution.
... These dual AGN serve as essential targets for multiwavelength astronomical observations and offer crucial insights into the processes of black hole mergers and activations. For example, some observations suggest that galaxy mergers may trigger black hole accretion (e.g., Liu et al. 2012;Koss et al. 2012;Fu et al. 2018). However, recent surveys suggest that the stochastic accretion mode could play a dominant role even in the presence of kiloparsec-scale dual-AGN systems (e.g., Hopkins & Hernquist 2006;Gross et al. 2019;Steffen et al. 2023). ...
It is believed that dual active galactic nuclei (AGN) form during galaxy mergers. Studying dual-AGN emission can provide valuable insights into galaxy merging and evolution. To investigate parsec-scale radio emission properties, we observed eight radio components of four selected dual-AGN systems using the Very Long Baseline Array (VLBA) at 5 GHz in multiple-phase-center mode. Among them, two compact radio components, labeled J0051+0020B and J2300-0005A, were detected clearly on parsec scales for the first time. However, the radio emission of the other six components was resolved out in the high-resolution images. We provide the values or upper limits of the brightness temperature and radio emission power, and analyze the emission origins in detail for each target. Based on their physical properties reported in this work and in the literature, we suggest that the radio emission in J0051+0020B and J2300-0005A originates primarily from compact jets, while the other six sources show more complex emission mechanisms. In addition, our VLBA observations suggest that the systematic X-ray deficit in our dual-AGN sample is likely attributed to the tidally induced effect and possibly a viewing angle effect.
... another study of AGN fractions in MaNGA galaxies, which used close galaxy pairs to define the merger sample, found that 23.8% of mergers host AGNs while 14.5% of nonmergers host AGNs(Fu et al. 2018). The higher AGN fractions in that study are likely explained by the difference in for Fu et al. 2018) as well as the difference in AGN selection; Fu et al. (2018) selected AGNs via a combination of the [O III]/ Hβ versus [N II]/Hα BPT diagnostic (Baldwin et al. 1981) and the Hα equivalent width versus [N ii]/Hα (WHAN; Cid Fernandes et al. 2010) diagnostic. ...
To facilitate new studies of galaxy-merger-driven fueling of active galactic nuclei (AGNs), we present a catalog of 387 AGNs that we have identified in the final population of over 10,000 z < 0.15 galaxies observed by the Sloan Digital Sky Survey-IV (SDSS-IV) integral field spectroscopy survey Mapping Nearby Galaxies at Apache Point Observatory (MaNGA). We selected the AGNs via mid-infrared Wide-field Infrared Survey Explorer colors, Swift/Burst Alert Telescope ultra-hard X-ray detections, NRAO Very Large Array Sky Survey and Faint Images of the Radio Sky at Twenty centimeters radio observations, and broad emission lines in SDSS spectra. By combining the MaNGA AGN catalog with a new SDSS catalog of galaxy mergers that were identified based on a suite of hydrodynamical simulations of merging galaxies, we study the link between galaxy mergers and nuclear activity for AGNs above a limiting bolometric luminosity of 10 44.4 erg s ⁻¹ . We find an excess of AGNs in mergers, relative to nonmergers, for galaxies with stellar mass ∼10 ¹¹ M ⊙ , where the AGN excess is somewhat stronger in major mergers than in minor mergers. Further, when we combine minor and major mergers and sort by merger stage, we find that the highest AGN excess occurs in post-coalescence mergers in the highest-mass galaxies. However, we find no evidence of a correlation between galaxy mergers and AGN luminosity or accretion rate. In summary, while galaxy mergers overall do appear to trigger or enhance AGN activity more than nonmergers, they do not seem to induce higher levels of accretion or higher luminosities. We provide the MaNGA AGN Catalog and the MaNGA Galaxy Merger Catalog for the community here.
... Also, the SMBH accretion seems to be enhanced in pairs (Liu, Shen & Strauss 2012 ) relative to isolated galaxies. The fraction of AGN pairs was found to be higher than that expected from a random distribution (Ellison et al. 2011 ;Liu, Shen & Strauss 2012 ), and this fraction increases for smaller MNRAS 527, 6722-6731 (2024) separations between the pair members (Fu et al. 2018 ), suggesting a mutual triggering of AGN activity. Morphological signals of merging and tidal interactions also seem to increase the frequency of AGN (Alonso et al. 2007 ). ...
The large and small scale environments around optically-selected AGN host galaxies and a control sample of non-active galaxies in the MaNGA survey have been investigated in order to evaluate the importance of the environment in AGN triggering. Using the MaNGA integral field spectroscopy, we quantify non-circular motions of the ionized gas and detect an excess of radial gas motions in AGN hosts relative to control galaxies, not associated to AGN feedback and are most likely the result of tidal interactions, possibly associated with the triggering of the AGN. We find that the large scale environments are similar for the AGN hosts and control galaxies in our sample and are biased towards lower large scale densities and group virial masses, suggestive that the large-scale environment properties is only relevant to the AGN phenomenon in an indirect way, in the form e.g. of the morphology-density relation. The small scale environment as measured by the frequency and luminosity of close neighbours was also found to be similar for AGN and control galaxies. However, we find a correlation between the intensity of the non-circular gas motions in AGN hosts and the strength of the tidal field, while the control sample does not present such correlation. Also, AGN hosts with the most intense radial gas motions present larger tidal fields than their control galaxies. These findings indicate that at least a fraction of the AGN hosts in our sample have been triggered by tidal interactions with nearby galaxies.
... Galaxy mergers are expected to play a significant role in AGN triggering and fuelling mechanisms and the corresponding growth of a massive black hole (Mayer et al. 2010 ;Alle v ato et al. 2016 ). Observational results imply that the AGN activity depends on the separation between pairs (Satyapal et al. 2014 ;Fu et al. 2018 ;Dougherty et al. 2023 ), including the observation of rare dual-AGN (McGurk et al. 2015 ). There is evidence for the different behaviour observed in absorbed and unabsorbed X-ray AGNs (Guainazzi et al. 2021 ) with decreasing separations. ...
We present a sample of 99 dwarf galaxies (M* < 109.5 M⊙) with X-ray activity in their central regions. The sample was obtained from a match of the SRG/eROSITA X-ray catalogue in the eastern galactic hemisphere with the MPA-JHU SDSS catalogue. The obtained matches were cleaned rigorously with the help of external optical catalogues to increase the purity of the sample. This work is the largest study of this kind – X-ray activity in ≈85 per cent of matched dwarfs was not reported before. The majority of X-ray active dwarfs are identified as star-forming galaxies. However, the X-ray luminosity of 82 objects cannot be explained by the collective emission of X-ray binaries, rendering them strong candidates for dwarf galaxies with an active accreting black hole in their centre. We find that the fraction of AGN among dwarf galaxies drops from ∼2 · 10−2 at LX ∼ 1039 erg s–1 to ∼(2 − 4) · 10−4 at LX ∼ 1041 erg s–1 and increases with the stellar mass of the host galaxy. We serendipitously discovered sources with unexpected properties. We report on a tidal disruption event (TDE) candidate in a dwarf galaxy, a massive black hole in a dwarf galaxy with a soft thermal spectrum, a luminous dwarf galaxy with an obscured X-ray spectrum and a few other peculiar sources. We found three Ultra-luminous X-ray (ULX) source candidates and a sample of X-ray bright galaxy pairs, in four of which both members shine in X-rays.
... Gao et al. ( 2020 ) have shown that AGN is more likely to be found in mergers, and the ratio of AGN fraction in mergers relative to non-mergers is 1.81. Studies using MaNGA data show that tidal interactions can induce around 30 per cent more AGN than stochastically fueled AGN at projected separations of 10kpc (Fu et al. 2018 ;Steffen et al. 2023 ). Merger simulations also show enhanced AGN activity (Mihos & Hernquist 1996 ;Rupke, Kewley & Barnes 2010 ;Hopkins et al. 2013 ;Moreno et al. 2019 ). ...
We present a study of the morphology of star formation and the associated nuclear activity in a sample of 8 closely interacting southern galaxies, which are in different stages of interaction, starting with nearly merged nuclei that have one prominent bulge to more widely spaced interacting galaxies. We have used Far-Ultraviolet (FUV) observations from the Ultraviolet Imaging telescope (UVIT), near-Infrared observations from the infrared survey facility telescope (IRSF) and archival optical data from the VLT/MUSE integral field spectrograph. Analysing resolved stellar populations across the disk of the interacting galaxies can provide unique insights into how interactions affect galaxy properties, such as morphology, star formation rates and chemical composition. We take advantage of the unprecedented capabilities of MUSE and UVIT to carry out a highly detailed spatially and spectrally resolved study of star formation rate, star formation histories, metallicity and AGN activity in the sample of eight interacting galaxies which are in different stages of interaction. Most of our sample galaxies are gas-rich and show evidence of recent, massive star formation in tidal tails, rings and spiral arms. This is evident from their FUV and Hα emissions, which trace young, massive star-forming regions. We compared the star formation rate in the barred and unbarred galaxies in our sample and found that the barred galaxies do not show significant enhancement in star formation rate or large-scale difference in star formation morphology compared to unbarred galaxies. IC5250 and NGC7733N, show extended nuclear outflows of size ∼ 5 kpc and 8 kpc respectively.
... Gao et al. (2020) have shown that AGN is more likely to be found in mergers, and the ratio of AGN fraction in mergers relative to non-mergers is 1.81. Studies using MaNGA data show that tidal interactions can induce around 30 % more AGN than stochastically fueled AGN at projected separations of 10kpc (Fu et al. 2018;Steffen et al. 2023). Merger simulations also show enhanced AGN activity (Mihos & Hernquist 1996;Rupke et al. 2010;Hopkins et al. 2013;Moreno et al. 2019). ...
We present a study of the morphology of star formation and the associated nuclear activity in a sample of 8 closely interacting southern galaxies, which are in different stages of interaction, starting with nearly merged nuclei that have one prominent bulge to more widely spaced interacting galaxies. We have used Far-Ultraviolet (FUV) observations from the Ultraviolet Imaging telescope (UVIT), near-Infrared observations from the infrared survey facility telescope (IRSF) and archival optical data from the VLT/MUSE integral field spectrograph. Analysing resolved stellar populations across the disk of the interacting galaxies can provide unique insights into how interactions affect galaxy properties, such as morphology, star formation rates and chemical composition. We take advantage of the unprecedented capabilities of MUSE and UVIT to carry out a highly detailed spatially and spectrally resolved study of star formation rate, star formation histories, metallicity and AGN activity in the sample of eight interacting galaxies which are in different stages of interaction. Most of our sample galaxies are gas-rich and show evidence of recent, massive star formation in tidal tails, rings and spiral arms. This is evident from their FUV and H emissions, which trace young, massive star-forming regions. We compared the star formation rate in the barred and unbarred galaxies in our sample and found that the barred galaxies do not show significant enhancement in star formation rate or large-scale difference in star formation morphology compared to unbarred galaxies. IC5250 and NGC7733N, show extended nuclear outflows of size 5 kpc and 8 kpc respectively.
... In particular, dedicated efforts have been put into searching for DQ candidates at a few kpc scales with double-peaked features of [O III] (e.g. Liu et al. 2011 ;Fu et al. 2018 ), although it has been pro v ed only a small fraction of double-peaked targets are genuine DQs (e.g. Shen et al. 2011 ;Comerford et al. 2015 ). ...
There are some strange quasars with multiple Gaia detections or observed with abnormal astrometric characteristics, such as with large proper motions or significant astrometric noises. Those strange quasars could be potential candidates of quasar-star pairs, dual quasars (DQs), or lensed quasars (LQs). Searching for both DQs and LQs is of great importance in many fields of astrophysics. Here in this work, we select 143 SDSS spectroscopically confirmed quasars that have multiple Gaia EDR3 detections within 1 arcsec of the SDSS quasar’s position. We apply several optical identification methods to classify this sample. We firstly exclude 65 quasar-star pairs via their stellar features including their parallaxes and proper motions, stellar features in the SDSS spectra, or via the colour-colour diagram. Based on the spectral-fitting results, we find 2 DQ candidates, one of which presents a double-peaked [O III] emission line feature and the other shows a broad Hβ velocity offset (∼ 870 km s−1) relative to the [O III] λ5007 line. Via the colour difference method, we further find 56 LQ candidates with similar colours in their multiple images. We also cross-match 143 objects with the HST archive and find 19 targets with archival HST images. Our classification results of those 19 targets are mainly consistent with previous works.
