Pos(Meerkat2016)008 , 12 , , 5 8 and I in the I , 2 1 Kpc; Measure , S

PoS(MeerKAT2016)008 , 12 , , 5 8 and I in the I , 2 http://pos.sissa.it/ 1 kpc; measure , S. I. Loubser 5 Mpc from the . 4 ∼ 1 , R.-J. Dettmar 10 kpc. 7 ∼ , R. Pizzo ∼ 3 morphology of resolved , J. H. van Gorkom I 3 ; and attempt to detect H

at a resolution of M 2 5 − 10 at a resolution of , R. F. Peletier cm , S. C. Trager × 3 2 , 5 − 2 19 13 , S. Colafrancesco 6 ∼ , , R. C. Kraan-Korteweg cm 5 ) I 11 , 18 10 (H 10 , 9 M ∼ reaching a projected distance of 2 , G. L. Bryan 12 deg , M. W. L. Smith 4 , T. A. Oosterloo , 9 1 3 ∼ , 2 , G. I. G. Józsa 1 mass function down to I 3 , L. Richter , M. Murgia 4 , 3 , 3 , 2 2 , F. Govoni 4 , W. J. G. de Blok 1 , ∗ [email protected] Speaker. radio continuum survey of theMeerKAT. Fornax is Fornax the second galaxy most cluster massive cluster toin within the be 20 Mpc southern carried and hemisphere. the out largest Its withwhere nearby low cluster most the X-ray galaxies luminosity SKA makes live precursor it andgrowth representative where of makes substantial the it galaxy environment evolution angas takes excellent accretion place. laboratory and Fornax’s for stripping ongoing processes studying in and galaxies the the falling neutral assembly medium in of in theWe the clusters, cluster, cosmic will the web. and observe physics the a connection of regioncluster between of centre. these This willcluster, cover where gas-rich a in-falling wide groups are range found. of Wegalaxies will: down environment study to density the a H out column density tothe of the slope a outskirts of few the times of H 10 the cosmic web reaching a column density of We present the science case and observations plan of the MeerKAT Fornax Survey, an H ∗ Department of Physics and Electronics, Rhodes Centre for Radio Astronomy Techniques and Max-Planck Institut für Radioastronomie, Auf demCentre Hügel for 69, Space D-53121 Research, Bonn, North-West University, Germany PotchefstroomSchool 2520, of South Physics Africa and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA, UK Copyright owned by the author(s) under the terms of the Creative Commons INAF - Osservatorio Astronomico di Cagliari,ASTRON, Via Netherlands della Institute Scienza for 5, Radio 09047 Astronomy, SelargiusKapteyn Postbus (CA), 2, Instituut, Italy NL-7990 University AA of Dwingeloo, Groningen, PO NL Astronomy Box Department, 800, University NL-9700 of AV Cape Groningen, NL Town,Department Rondebosch of 7700, Astronomy, Cape Columbia Town, University, South Mail Africa Code 5246, 550 West 120th Street, Center for Computational Astrophysics, Flatiron Institute, 162 5th Ave, 10010, New York,School NY, of Physics, University of theAstronomisches Witwatersrand, Institut 2050, der Johannesburg, Ruhr-Universität South Bochum, Africa Universitätsstr. 150, D-44780 Bochum, SKA South Africa, 3rd Floor, The Park, Park Road, Pinelands 7405, South Africa c 1 2 3 4 5 10027, New York, NY, USA 6 USA 7 8 Germany 9 10 Technologies, Rhodes University, PO Box11 94, Grahamstown 6140, South Africa 12 13 E-mail: M. A. W. Verheijen M. Ramatsoku F. M. Maccagni Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). B. S. Frank MeerKAT Science: On the Pathway to25-27 the May, SKA, 2016, Stellenbosch, South Africa The MeerKAT Fornax Survey P. Serra PoS(MeerKAT2016)008 P. Serra ]). The morphology-density 5 , 4 ) gas in Fornax. This is the gas I ]). The large range of densities where 2 , ]) indicate that, in dense environments, 1 7 , 6 1 gas is that it can be detected all the way out to the I can indeed reveal on-going episodes of gas removal as well I ). 1 gas removed from galaxies living in Fornax. We will study the detailed I ] and since then revisited by numerous authors (e.g., [ 3 Detect the tails of H physics of gas removal from galaxies ofwithin different mass this and type cluster, as and a quantify functionevolution of the of their impact these position objects. of these gas stripping events on the subsequent We will use MeerKAT to observe the neutral hydrogen (H The main goals of the MeerKAT Fornax Survey are to: The goal of the MeerKAT Fornax Survey is to study the physical processes that drive the The clearest manifestation of the importance of environment for galaxy evolution is that red, • relation and its evolution across cosmic time (e.g., [ phase from which molecular gasstand and galaxies. new stars A form, crucialoutskirts and property of is of galaxies. therefore the These a H regions keyoffer are observable a the to privileged interface under- view between of galaxieshigh and the their sensitivity way environment, cold and and gas resolution, flowsas H in accretion. and out Such of directinfluences them. galaxy evidence evolution. If is imaged of with paramount sufficiently importance to understand how environment evolution of galaxies ingalaxies the lose their densest cold gas, regions and of why doin the they action stop cosmic accreting by fresh observing web, gas? the We galaxy willis flow study clusters. an of these processes ideal cold target gas How because inside doMeerKAT of a observations these its (Table particular proximity, cluster size of and galaxies, evolutionary Fornax. state, Fornax and is perfectly located for galaxies tend to quickly loseOn their the cold contrary, gas, in stop low-densityaccreting forming environments, fresh new galaxies gas. stars can and hold This become gas oncolour, red clumpy is to appearance and then their and smooth. converted cold – into since gas newUnderstanding gas and/or stars, the is keep cause giving typically of distributed late-type the on galaxies strong ain their connection disc which blue between – they individual their galaxies are flattened and shape. embedded thephysics. – cosmic the web very structure of the Universe – is at the core of modern astro- gas-poor early-type galaxies become more common, andmon, blue, with gas-rich increasing late-type galaxies environment less density. com- Thiscovered by is [ the morphology-density relation originally dis- The MeerKAT Fornax Survey 1. Background and main goals of the MeerKAT Fornax Survey Galaxies form and evolveintersecting at sheets favorable and filaments locations of ofearly matter Universe the which and evolves originates cosmic under from the web pull weak ofgalaxies – density gravity form (e.g., fluctuations a [ and in live large-scale the in network thetheir of environment: cosmic the web temperature corresponds and to pressurethe of a the number broad surrounding density variety inter-galactic of of gaseous galaxies; medium; physical andgalactic conditions the medium. in motion These of conditions galaxies have relativefor to a star one strong formation another effect – and on in to the and the flow out inter- of of cold galaxies gas and, – therefore, the on raw their material evolution. PoS(MeerKAT2016)008 . 19 ]).

10 16 M 5 × ]), and P. Serra 5 10 15 , ∼ × 5 14 and ∼ 18 10 ∼ as well as stars from the outer I ] ] ] ] ] 11 12 13 12 12 [ mass detection limit of I

M erg/s [ 13 41 0.7 Mpc [ 35d 30m 10 2 370 km/s [ 10 − × × 7 5 Key properties of Fornax X σ vir L dyn RA 3h 38m R Dec ]). As galaxies move within a cluster the hot medium exerts a 1 kpc, and with an H M scale 10 arcsec/kpc 18 ∼ Table 1: removal is related to the fact that the volume between galaxies is distance 20 Mpc [ I 10 to gas which, according to cosmological simulations, should be found be- ∼ I mass function in Fornax. We will measure how much gas is contained in small I ]). With the MeerKAT Fornax Survey, we will start pursuing these goals already in 10 , 9 , 8 tween galaxies in the cosmicthe web. first images This and is velocity the fields most of challenging this gas goal, component potentially across providing hundreds of kpc. Study the H galaxies and is available tocompare be our captured results by to those larger obtained ones in fuelling lower- star andDetect higher formation, the density and environments. faint we H will at resolutions from Tidal stripping of cold gas is observed frequently in groups of galaxies (e.g., [ A second mechanism of H 2 • • − 2. The fate of cold gas in clusters 2.1 Hydrodynamical and tidal effects Using the new MeerKAT data weence will the study flow of a cold wide gas variety inrelation. and of out physical of First, processes galaxies, as and which are the can theume. influ- environment likely drivers density This of implies increases the an morphology-density so enhanced doesbetween chance the of them. number encounters of and, During therefore, galaxies interaction these perregions (or of unit events even vol- galaxies, merging) tidal reducing forces theiralso can future trigger remove ability strong H to star formation formof activity, stars. which the interacting can In systems. quickly extreme exhaust cases the these initial forces cold can gas reservoir cm the early phase of MeerKAT’s life.from We will its do centre so (projected), by reaching mosaicking the a Fornax column region density out sensitivity to between 1.5 Mpc These are all key science goalscase spelled ([ out in the recently revised Square Kilometre Array science there are strong indications thatHowever, it this is stripping at mechanism work is also inefficientanother. when in galaxies the Therefore, move outskirts it at of high is big speedclusters expected clusters relative of to to like high become one Virgo mass. ([ less important towards the centre offilled clusters with and a in hot gaseous medium.that it In can the be densest detected regions in of X the rays cosmic ([ web this medium is so hot The MeerKAT Fornax Survey PoS(MeerKAT2016)008 ] ∝ of 20 ρ ram ], this P P. Serra ]). [ 25 ]), Coma 19 ] around a 16 26 from a galaxy I 1 Gyr. ∼ in I ]. According to [ 24 discovered by [ I ]). The orbit of the stripped galaxy is observations for these studies. 17 I . (Image credits: P.A. Duc.) 2 − cm with which galaxies move through it ( 20 v ], Fig. 1). Modelling suggests that this type of 17 3 ]). ]). Furthermore, the cold gas of galaxies could undergo ther- 23 27 column density is below 10 ]). The strength of ram pressure grows linearly with the density I 22 reveals with remarkable clarity the direction of motion of the galaxy relative I grow with cluster mass and, therefore, ram-pressure stripping is expected to be from galaxies. However, other processes are at work too. For example, the large- v I and (light blue) on top of an optical image of HCG 44 ([ and stars from the outskirts of galaxies, as proposed by [ I ρ I H tail around the galaxy group HCG 44 ([ I Ram pressure stripping has so far been detected in massive clusters like Virgo ([ Galaxy tidal interaction and ram-pressure are the most frequently discussed mechanisms for Additional stripping mechanisms are, again, related to the presence of hot gas between galax- ). Both ]) and Abell 1367 ([ 2 v 21 show a particularly convincing example ofmorphology this of process the in H the Virgo cluster,to NGC the 4522, hot where medium. the Such cases highlight the uniqueness of H small group of galaxies.giant Another H system which may have formed through this mechanism is the the removal of H scale gravitational potential of groups ormerging clusters groups of or galaxies clusters) (or even exerts the tidalremove time-varying forces H potential on of galaxies that move through it. These forces can tidal stripping can be fast and efficient, removing large fractions of the H Figure 1: shown by the red line. The H ram pressure on their gas but not on their stars, resulting in the stripping of gas alone ([ ([ the hot medium and quadratically with the velocity may well be the origin of the famous Leo Ring, a giant ring of H The MeerKAT Fornax Survey ρ efficient in big clusters. On theclusters contrary, or evidence groups of of ram galaxies pressure (e.g., has [ so far been weak in smaller ies. For example, viscosity and turbulence can contribute to the stripping of H moving through the hot medium ([ PoS(MeerKAT2016)008 ) I ]) 42 (H mass I ]); and P. Serra M 36 , ]) and Abel 35 , 16 34 , 33 ]); the role of magnetic to, e.g., ram pressure or 30 I ]). Indications of both types 28 ]); the possible enhancement of ] obtain results more in line with 32 39 , 31 even in the presence of weak stripping I mass function I 4 H ]). Our MeerKAT survey, with its combination of ] find no significant difference between samples of 37 41 ]). As with ram pressure, the expectation is that these 16 ]), suggests that the mass function is flat and low- , 43 29 ] and [ 40 ] report an opposite effect (i.e., a steeper slope and a higher fraction 38 mass in denser environments), while [ I -poor, large galaxies will progressively lose all their H I ]). In some cases the two types of stripping may even work together: gas could be moved accretion from the cosmic web 22 I The reason why small galaxies could be particularly gas-poor in clusters is that, having a shal- In summary, the relative strength of the processes described above changes as a function of Gas stripping from hydrodynamical and tidal forces, and its possible effect on star formation in H low gravitational potential, they cannot hold on to their H tidal forces without being able to accrete new gas – hence ceasing forming stars. and for a samplegalaxies of are local rare groups in ([ atcase least in some Fornax too. dense environments. Our data will2.3 establish whether that is the According to modern cosmology, clusters like Fornax are situated at the intersection between fila- of objects with a low H galaxies living in different environments.in Finally, the the careful nearby analysis large-scale of structure individual using over-densities sensitive data, as done for the Ursa Major cluster ([ environment density: tidal forceshigh-density and environments, ram respectively. pressure However, shouldoverlap observations between be suggest the the that two, dominant there such effects is as in significant at low- the and outskirts of massive clusters like Virgo ([ mechanisms play a much bigger role inside massive clusters than in small clusters and groups. fields in reducing the efficiency of ram-pressure stripping ([ forces. An effective way tofunction test in this clusters expectation is to to thatcontradictory. compare For in the example, lower-density [ faint-end environments. slope of Results the so H far have beenthe surprisingly expectations. Furthermore, [ galaxies, have received significant attention from theoristing and aspects simulators that in are recent being years. activelyrelative Outstand- debated to include: large the galaxies efficiency of in gas groups stripping and of clusters small galaxies of different mass (e.g., [ to large radius by tidalgravitational forces binding and to the be galaxy. susceptible to ram-pressure stripping because of its weaker sensitive spectral-line and radio continuum dataconstraints (see on below), these will simulations. provide important observational 2.2 Removal of gas from small galaxies:An the interesting effect ofenvironments the may various be gas devoid stripping ofcaptured, processes small, they described gas-bearing can above galaxies. progressively is refill Theseclusters that the are are high-density gas important reservoir H because, of when larger galaxies. If all small galaxies in The MeerKAT Fornax Survey mal evaporation by interacting withof the stripping hotter, are surrounding found gasbut ([ inside low-surface-density the gas Virgo discs cluster, ([ where some galaxies are surrounded by regular 1367 ([ star formation in stripped galaxies ashow well to as use within the high-resolution tails simulationssemi-analytic of and models stripped gas observations of ([ to galaxy calibrate evolution the ([ recipes implemented in PoS(MeerKAT2016)008 I I ] 10 P. Serra 10 kpc over a ∼ ]) its full distribution 45 signal from the cosmic web ]). Although neutral gas has I , most of what we know about 44 I 1000 times less dense than the H . Indeed, while a few dozen clusters I > at the ideal resolution of 2 − cm and below ( 5 18 2 in emission – have never been studied before ([ 10 − I ∼ cm ] even suggest that the cluster itself and a nearby galaxy 18 48 10 . Single-dish radio telescopes can reach lower formal column ]). [ 2 ∼ − 47 ]; see Fig. 1). Additional examples are some even more massive , cm 16 46 , 20 percent of all galaxies in the Universe live in clusters this large. All 19 49 in the cosmic web is extremely challenging because this gas is expected ∼ I , our survey of the Fornax cluster is well positioned to attempt the detection 2 ]). With a sensitivity of ]). Only 10 22 , 21 The other crucial point is that Fornax represents an important class of dense, low-mass clusters The detection of H can be diluted ([ densities but the resolution is so poor (many tens of kpc) that the H found inside star-forming galaxies). In contrast, theimages typical is sensitivity of of current a interferometric H few times 10 other galaxies live in less dense regions of the cosmic web and evolve in very different conditions. have been observed at limited sensitivitythe and detailed physics poor of resolution cold in gas stripping H of in just high-density a environments handful comes of from clusters the –very observation all nearby much Virgo more (e.g., massive than [ Fornax.clusters The such most as notable Coma example is and the distance Abell ([ 1367, whose study is however hampered by the ten times larger where many galaxies live but which are poorly studied in H group (centred on NGC 1316)making are this falling an towards extremely each exciting other regioninvolved to along in study. a this Our filament process MeerKAT of of survey will cluster thesee cover growth cosmic Sec. the – web, 5 full including – region the allowing cluster us centre to catch and the the effect NGC of 1316 cluster group; assembly on galaxy evolution in action. to have very low column density, and imaging of this elusive gas component in a cluster. 3. The importance of Fornax Fornax is an extremely important systemFirst, for it the is study very of nearby galaxy –(Table evolution the 1). in second dense most environments. This massive galaxy meansmarised concentration that in within the Sec. 20 Mpc processes after 2very driving Virgo can active galaxy be evolutionary evolution state. studied in atlarge dense This galaxies a environments fact in unique sum- Fornax is resolution are sometimes of andalready overlooked early quite sensitivity. in morphological evolved. Yet, type the Second, observations – demonstrate literature Fornax indicating thatof because is Fornax that new is most the in gas-rich currently cluster a galaxies growing as by and a accretion just galaxy whole joined groups, is the and cluster there (e.g., is [ evidence that many dwarf galaxies have been detected in absorption alongand a kinematics limited – number only of accessibleand QSO through references sight-lines therein). H ([ survey area of 2 Mpc The MeerKAT Fornax Survey ments of the cosmic web. These filamentstowards are galaxies filled and with hydrogen feed gas, their whichfrom continuous is the expected growth to cosmic through stream web star is formation.On a the Such fundamental one and accretion hand, yet of it highly gas On seems controversial the to other aspect be hand, of required attempts modern to to imageThis cosmology. explain this is the gas rate partly in the of due nearby galaxy the Universeagainst growth have fact ionising so across that radiation, far cosmic been and the time. unsuccessful. most density of of the gas gas in should the be cosmic ionised web ([ is too low for self-shielding PoS(MeerKAT2016)008 and ]) and 13 P. Serra 56 10 detection , I ∼ 55 ]). Using our sensitive MeerKAT data we 59 6 ]). Our sensitive data will result in the H 58 , ]). The intracluster medium regulates the expansion of 57 61 ]. and radio continuum imaging will provide insights into the I 63 ]). The Fornax cluster is the best target within this mass range, 53 , 52 , 8 studied by [ ]). Deep H , I 62 51 , picture, and make a crucial contrast to massive clusters. The goal of our project ]). Therefore, low-velocity galaxy encounters are much more frequent, and the 50 I 54 (e.g., [

M Deep continuum data will also provide an ideal dataset to study AGNs in Fornax. The link Radio continuum emission not associated with specific galaxies will also be of great interest A final, interesting aspect of Fornax is that it will allow us to study the cold gas content In the less massive Fornax cluster, the density of the intra-cluster medium and the velocity 14 between radio AGNs and theticularly environment important in in which clusters, theyinfluence where are each radio embedded other galaxies is profoundly and (e.g. very the tight X-ray-emitting [ and intracluster is medium par- too. Indeed, synchrotron cluster radio relicsemission represent and the are most directly spectacular connected example to of the clusterdiffuse dynamics radio of and galaxy extended clusters. radio These optically sources unidentified are detected at the cluster peripheries, where they trace shock will be able to investigate this phenomenonenhancement further. of Moreover, star-formation we rate will due be able to to ram study pressure. the possible effects of Fornax A on theX-ray surrounding emission cold and gas, H further investigating the mix of radio continuum, radio galaxies and affectssame their time, morphology the by radio lobes confining maycontinuum and inflate source distorting cavities in in the the our radio intraclusterFornax field lobes. medium. A is is The well Fornax At most known notable A, for the radio itsrays which large in resides radio lobes in the and the cluster was recently south-west ([ discovered to infalling be sub-group. injecting cosmic importance of tidal interactions relative tooffers therefore ram-pressure the should unique possibility be to significantly extend increased. theobservational baseline H Fornax of clusters for which weis have a to detailed perform exactly this comparison between Fornax and more massive clusters. of the many ellipticalspirals, and these lenticular galaxies galaxies do in contain the some cluster. cold Although gas typically both gas-poorer within than and outside clusters ([ dispersion of galaxies are 2times times larger lower ([ than in Virgo, while the number density of galaxies is 2 The MeerKAT Fornax Survey In particular, substantial exhaustion ofmorphological galaxies’ transformation cold appear gas reservoir, to star occur10 formation in quenching dark-matter and halos ofwhile mass the more between massive clusters studied so far (e.g., Virgo, Coma) are well above it. the comparison between gas andaccretion stellar and morphology removal and in kinematics these objects revealsof ([ a numerous clear such pattern galaxies in of Fornax. gas 4. Radio continuum and polarisation Our data will provide excellentStar sensitivity forming to galaxies give radio rise continuum toelectrons emission radio in synchrotron from supernovae. emission galaxies This through emission in the correlates Fornax. productionthe tightly of with heating relativistic the far-infrared of emission, dust connecting their by inter-stellar massive medium stars this to correlationemission the at is the supernovae affected location rate. locally of the because strongest As of ram pressure cluster a ([ galaxies lower radio are continuum stripped of PoS(MeerKAT2016)008 I ]). the 66 × 5 P. Serra . 1 ∼ 25 kHz) channel. ∼ ]). The current knowledge 1 Mpc, which is 65 ∼ , 64 . The grey circles indicate galaxies 2 (P.I. Serra). Colours represent the heliocentric

. Open, down-pointings triangles indicate new H M

7 7 M 10 8 ]. The size of the circles is proportional to the logarithm × 10 5 60 × ∼ 3 ∼ ] down to 47 by [ I detections. The dashed magenta circle has a radius of I down to a natural r.m.s. noise level of 0.1 mJy/beam in a 5 km/s ( 2 MeerKAT Fornax Survey layout. North is up, east is left. The small black crosses represent 86 12 deg Finally, regardless of the detection of diffuse radio continuum emission from within the cluster, ∼ about cluster radio relics is still limited and only a few examples are reported in the literature ([ of galaxies’ B-band flux.to The the two east) large and red of crossesgalaxies the indicate detected south-west the sub-group in (NGC location H 1316, of to the the cluster west). centre Solid, (NGC up-pointing 1399 triangles indicate we will be able tothousands background measure polarised the radio Faraday sources – rotationfield resulting caused in in the by a cluster the characterisation with of Fornax’the a the magnetic first the resolution field magnetic time of for the a a few propertiesmagnetic tens few of fields of in galaxies kpc. which and they the This are is embedded. intra-cluster adequate medium to in start Fornax connecting with5. for those of Survey strategy the In order to reach the scienceof goals summarised in Sec. 1 we will use MeerKAT to mosaic a region Figure 2: individual MeerKAT pointings. The40 solid percent and higher dotted than blue theweighting). contours minimum represent The noise noise solid in blue levels thelisted 10 contour mosaic as defines percent (0.1 definite a and mJy/beam or mosaic in likely area a cluster of 5 members 11.8 in km/s deg [ channel with natural The high sensitivity achieved by ourstudy the observations polarisation of properties Fornax of) will relic have sources the in potential this to dynamic, image low-mass (and cluster. The MeerKAT Fornax Survey velocity of the H waves deriving from the infall of gas and merging of sub-clusters ([ detections obtained with the ATCA down to virial radius (Table 1). PoS(MeerKAT2016)008 5 10 100 in the × ∼ 3 kpc) P. Serra I 5 ∼ detections ∼ I ]) is 5 Mpc (radius), . mass function in 0 67 I column density of tails formed in past I ∼ 30 arcsec ( I ∼ ; e.g., [ 110

M 1) this number goes down to 100 7 − 10 = 90 coverage per mosaic pointing. As ∼ 80 uv slope 70 1 kpc (Table 1). 1 kpc), allowing us to detect and study the ∼ 60 ∼ ) sensitivity of our survey within a 25-km/s line I 50 8 and below) at the appropriate resolution of (H 2 Bmin (arcsec) − 40 M σ 22 K for the 64 13.5-m MeerKAT dishes, this requires cm 30 10 percent calibration overhead. = 10 arcsec ( 18 ∼ 20 ∼ ]), and based on the number of known massive H column density and mass sensitivity to reveal episodes of gas robust = 0, tapering from 0” to 120” in steps of 10” 7 Mpc towards a gas-rich group to the south-east, and a larger . 10 I 68 0 ∼ 0 efficiency 3; [ 20 19 18 mass function of Fornax is the same as that in the field down to this . /

I

1 10 10 10

HI 5km/s) 25 , σ (3 sys N − mass function and attempt the first detection and imaging of H T I = 5 Mpc towards the infalling south-west group dominated by the peculiar . 1 at a resolution of ∼ 2 slope − detections. In case of a flat mass function ( I cm 10 kpc). Expected column density sensitivity as a function of angular resolution. Different angular res- 19 ∼ 10 150 H Fig. 3 shows the column density sensitivity within the survey area as a function of angular With optimal angular resolution, the 3 The survey footprint is shown in Fig. 2 and includes the cluster central × . Assuming that the H ∼ 5 60. Of course, measuring the number of detections and the slope of the H 900 h of telescope time including a

from the Parkes and ATCAof telescopes in the survey area∼ (twenty; see Fig.Fornax 2), is we precisely predict one a of total the key goals of our survey. In this respect, these predictions serve the sensitivity (i.e., M Figure 3: olutions are obtained taperingperformed the in visibilities CASA. at At the fixed distance Briggs of weighting Fornax, 10 (robust arcsec = 0). The simulation was resolution. This wasadopted obtained the by most performing recent a MeerKAT simulation specs and with the the planned CASA package, where we plus a small extension outextension to out to galaxy NGC 1316. Thedistances velocity from range the covered cluster by along the our line data of allow sight us (see to below). reach significantly larger required by our science∼ goals, our MeerKAT data will be sensitive to anwe H will have excellent sensitivityinteractions and and gas will stripping be events. ableexpected for Finally, to we gas detect in will the the start cosmic faintestarcsec to ( web H explore (10 the column density regime ∼ detailed morphology of gas in galaxies. Furthermore, at a resolution of width (appropriate for dwarfs with a total baryonic mass of The MeerKAT Fornax Survey This will deliver the requiredstripping, H study the H cosmic web. Assuming PoS(MeerKAT2016)008 2 tail in P. Serra I recessional I detections at ]) we will go I 28 mag/arcsec 47 detections com- I and radio contin- ∼ features (and vice ]) covering our full 0. I I a Herschel survey of 70 = ii) z at ]); I 71 several observations of the CO iii) ]); detections – whose rotational velocity the FDS survey, a deep optical imaging 73 I , i) 72 , covering the full range of galaxies in the 1 − 9 in the background of Fornax). Our MeerKAT mosaic I better resolution) of our MeerKAT survey compared to of the cluster and resulted in the detection of cold dust in 3500 kms × properties of the faintest galaxies in the cluster, including 2 + I 10 ∼ ]), SAMI (P.I. Scott) and MUSE (P.I. Sarzi). 74 (and even lower in projection) our spectral-line data will have an 1000 to 1 kinematics of the smallest H − I 1 km/s. We will obtain data at this resolution across an H − ∼ ) and we will increase the linear resolution by almost two orders of mag- observations carried out with the Australia Telescope Compact Array (P.I. I I (H 20 kms M ∼ integral-field spectroscopy of dwarf and giant galaxies in Fornax with a variety of bands (and even deeper with moderate smoothing of the images); this survey provides i better sensitivity (and ] (Fig. 2). Importantly, these new detections were found in the proximity of known ]). The higher angular resolution of the MeerKAT data will be fundamental to uncover iv) × 47 69 deeper in and r 100 × , g The recent ATCA survey is just one component of a large set of multi-wavelength observations In order to study the H To study the radio continuum emission (both in total and polarised intensity) and the magnetic ∼ velocity resolution of , -rich galaxies, indicating that there may be regions within the cluster where there is a larger 500 u I I H H the newly discovered large population of ultra-diffuse galaxies (e.g., [ velocity range of, at least, MeerKAT Fornax mosaic (and more) down toin a surface brightness sensitivity of versa), and to study the optical and H (J=1-0) molecular gas line inALMA galaxies (P.I. within Davis); Fornax together using with the ourwill Mopra MeerKAT build single-dish survey and a (P.I. Smith) the complete and Herschel census data,in of these the Fornax; observations cool interstellar mediuminstruments, (dust, including molecular WiFeS gas ([ and atomic gas) available for this cluster. The most recent efforts include: nitude. More recent H more such systems and understand their origin within Fornax. a key dataset to look for the optical counterpart of low-surface-brightness H Serra) had already improved the situation, allowing us to make make six new H cluster. These data are within the RFI-protected frequency range for H ∼ pared to [ availability of cold gas. Those same regions may thereforethe harbour ATCA one. many The more other H importantFornax result ([ of the ATCA survey is the first detection of an H survey carried out with OmegaCAM on ESO VST Iodice (P.I.’s and Peletier; [ Fornax, which covers the central 1630 deg galaxies of both early- and late morphological type ([ of the Fornax region will be Nyquist sampled at the highest observing frequency6. of 1670 Multi-wavelength MHz. observations of Fornax Our MeerKAT data represent a significant step forward for the study of H fields in the Fornax cluster900 we to will 1670 take MHz. data Thecommensal over use 25 a of kHz 770-MHz-wide our resolution data band of (e.g., in these to the study data H frequency will range facilitate RFI flagging and allow the The MeerKAT Fornax Survey sole purpose of showing thatthe we range will of be values discussed sensitive in tofunction the slope variations literature. will of be Based the well on mass below the 10 function above percent. slope numbers, within the error oncan the be mass as low as uum emission in the Fornax cluster. Compared to previous Parkes observations ([ the PoS(MeerKAT2016)008 I I ) ) 2 I I − iii) will (H (H study cm 2 1 kpc) ]); and P. Serra M M i) 19 ∼ 76 10 12 deg ∼ 20 Mpc, along ∼ ], which could ∼ 12 and a resolution of ]), rich groups like 2 81 -poorer and transition − I cm surveys, which target from I 18 mass of spirals becomes pro- mass function down to 10 I I ]). In addition, the ASKAP H ∼ 54 ]). However, it was only thanks to properties of galaxies living in such I 78 ]); iv) archival WISE images ([ 75 mass could be linked to the shrinking of the I at a 30 arcsec resolution. ]) to small groups (e.g., [

observations in galaxy clusters demonstrates the 10 M 80 I 7 represents a unique, direct tracer of these processes in 10 I × 3 ]). ), H 2 ∼ 20 − ) I 5 Mpc from the cluster centre (and much larger, cm . (H 1 19 M ∼ and below we can quantify variations in the mass-function slope. This

]) will provide complementary data on the larger-scale distribution of H ]). Comparing and contrasting the H M 77 in the cosmic web at a column density of 6 21 1 kpc, hunting for signs of gas stripping throughout the cluster and allowing I , ]). Finally, by pushing the sensitivity to low column density, we have been able ∼ 16 ]), small clusters like Fornax (this project), and clusters of larger size like Virgo ]); iii) archival UV GALEX imaging ([ 79 disc size and mass ([ , which we will then compare to values found in different environments; and I 42 48

M 5 morphology of resolved galaxies down to a column density of a few times 10 I Within this context, the MeerKAT Fornax Survey will provide the most accurate view of the The lesson of these developments is that, if imaged at sufficiently high resolution ( In addition to these new projects, several older campaigns resulted in valuable datasets which × discs (e.g., [ and radio continuum properties of galaxies in the Fornax cluster. Our mosaic of detect large numbers of dwarfs and measure the slope of the H 5 10 kpc. In the future, observations of this type will become routine over much larger areas and I I H H the H ∼ attempt to detect H from a late- to anposition early-type in morphology the through a cosmic varying web. balance of The processes history as of a H function of gressively lower as they approach a cluster’s centre (e.g., [ low-density regions of the cosmic web (e.g., [ different environments is key to obtaining a coherent picture of galaxy evolution. reach a projected distance of the line of sight) and coverwhere a gas-rich wide in-falling range groups of are environment found. density The out sensitive to MeerKAT the data outskirts willat of allow a us the resolution to: cluster, of a comparison to the distributionii) of other components of galaxies (e.g. stars, dust, molecular gas); ∼ over a larger range of environments with the Square Kilometre Array. importance of combining good column densityInitial sensitivity low-resolution and observations resolution led to to study the these conclusion processes. that the H and Coma (e.g., [ to directly see the faintthe gas reduced being H removed from the disc outskirts, i.e., witness the very cause of be expanded to targetscluster selected core ([ from our new VST images; ii)survey WALLABY Chandra ([ X-ray imagingin of the the Fornax region down to 7. Summary Decades of research onshaping galaxies their have gas formed content. a We expect tentative galaxies picture to of become the progressively H role of environment in higher-resolution images that such decrease of the H and sensitivity (a few times 10 action because it can reveal tailsdetection of limits stripped of gas 10 and truncatedis gas the discs, motivation while for by a reaching large number of completed and planned deepUrsa H Major ([ will complement our radio data. For example: i) the spectroscopic survey of [ The MeerKAT Fornax Survey v) HST/ACS imaging of the 40 brightest galaxies in Fornax ([ PoS(MeerKAT2016)008 D ]. 3 , 52 , P. Serra (Feb., 281 The ApJS 529 , ApJ The ATLAS , Observations ApJ , The Evolution of the Simulations of the Evolution since z = 0.5 The SKA view of the astro-ph/0005171 ,[ (June, 2005) 629–636 (Dec., 1997) 577–591, ]. ]. 435 X-Ray Emission from the Fornax 490 Advancing Astrophysics with the Advancing Astrophysics with the , , ]. ApJ Nature ]. , , 1501.01295 1501.01077 (Oct., 2000) 673–683 HI synthesis observations of the high-redshift 1104.3545 Substructure and Dynamics of the Fornax Cluster 542 ,[ 11 A survey of galaxy redshifts. IV - The data ApJ , Advancing Astrophysics with the Square Kilometre Array ]. ´ c, R. M. McDermid, P. Serra, K. Alatalo et al., (Oct., 1984) 15–24. . , astro-ph/0012415 (Apr., 2015) 132, [ (Apr., 2015) 128, [ 139 ,[ A&A The morphology-density relation - The group connection , ]. ]. (Sept., 2011) 1680–1696 . . (Mar., 1980) 351–365 416 (June, 1997) 143–155. astro-ph/9908192 This project has received funding from the European Research Council (ERC) under ,[ 236 482 Galaxy morphology in rich clusters - Implications for the formation and evolution of (Apr., 2015) 129. (Feb., 2001) L139–L142 ApJ MNRAS ApJ , , , 548 astro-ph/9707232 astro-ph/0504097 (AASKA14) of the Intergalactic Medium and theSquare Cosmic Kilometre Web Array in (AASKA14) the SKA era galaxies in Stephan’s Quintet Neutral Interstellar Medium in Galaxies project - VII. A new lookrelation at the morphology of nearby galaxies: the kinematic morphology-density Hubble Space Telescope Key Project on thePopulation II Extragalactic Secondary Distance Distance Scale. Indicators XXVI. and The2000) the Calibration 745–767 Value of of the Hubble Constant Cluster ApJL Exploring Neutral Hydrogen and Galaxy Evolution with the SKA formation, evolution and clustering of galaxies[ and quasars Galactic Morphological Types in Clusters Square Kilometre Array (AASKA14) galaxies (June, 1983) 89–119 (June, 1984) 95–99 of the Morphology-Density Relation for Clusters[ of Galaxies [8] S. Blyth, T. M. van der Hulst, M. A. W. Verheijen, B. Catinella, F. Fraternali, M. P. Haynes et[9] al., E. de Blok, F. Fraternali, G. Heald, B. Adams, A. Bosma and B. Koribalski, [5] M. Cappellari, E. Emsellem, D. Krajnovi [7] G. Fasano, B. M. Poggianti, W. J. Couch, D. Bettoni, P. Kjærgaard and M. Moles, [3] A. Dressler, [1] J. Huchra, M. Davis, D. Latham and J. Tonry, [2] V. Springel, S. D. M. White, A. Jenkins, C. S. Frenk, N. Yoshida, L. Gao et al., [4] M. Postman and M. J. Geller, [6] A. Dressler, A. Oemler, Jr., W. J. Couch, I. Smail, R. S. Ellis, A. Barger et al., [10] A. Popping, M. Meyer, L. Staveley-Smith, D. Obreschkow, G. Jozsa and D. J. Pisano, [14] G. S. Shostak, R. J. Allen and W. T. Sullivan, III, [11] L. Ferrarese, J. R. Mould, R. C. Kennicutt, Jr., J. Huchra, H. C. Ford, W. L. Freedman et al., [13] C. Jones, C. Stern, W. Forman, J. Breen, L. David, W. Tucker et al., [12] M. J. Drinkwater, M. D. Gregg and M. Colless, the European Union’s Horizon 2020 research and innovation programme (grant agreement No 679627). References Acknowledgments. The MeerKAT Fornax Survey PoS(MeerKAT2016)008 , ]. , ]. P. Serra 403 Discovery ]. . , (Mar., 1982) (Jan., 1999) MNRAS 1209.4107 , Probing (Feb., 2005) 198 510 ,[ ]. The Vela Cloud: A (Mar., 1994) 357 0903.2690 ApJL ,[ 107 , MNRAS ]. VLA Imaging of Virgo Spirals , AJ , MNRAS , (May, 2009) 87–102 arXiv:astro-ph/0403103 (Dec., 2009) 1741–1816 VLA H I Imaging of the Brightest ,[ 499 The effect of ram pressure on the star 138 A very large array survey of neutral ]. (Jan., 2013) 370–380 1410.8161 AJ A&A , Massive HI clouds with no optical astro-ph/9912405 ,[ Discovery of a large intergalactic H I cloud , 428 ,[ (Jan., 2010) 102–119 . 1988. ]. VLA H I Observations of Gas Stripping in the 139 . 1409.3486 MNRAS AJ 12 , , Gas and dark matter in the Sculptor group: NGC 55 ,[ ]. . . ]. (June, 2004) 3361–3374 ]. 1307.2962 ,[ 127 (Feb., 2015) 969–992 ]. (Feb., 2000) 580–592 AJ Star formation quenching in simulated group and cluster galaxies: Ram pressure stripping in elliptical galaxies - II. Magnetic field , 447 On the Infall of Matter Into Clusters of Galaxies and Some Effects on Thermal evaporation of gas within galaxies by a hot intergalactic 119 (Oct., 1983) L1–L5 1408.4521 1001.3900 The Ties that Bind? Galactic Magnetic Fields and Ram Pressure Stripping ,[ (Aug., 1972) 1–+ AJ , 273 ,[ MNRAS 176 , (Apr., 1977) 501–503 (Dec., 2014) 1997–2014 ApJL , ApJ 266 445 , Transport processes and the stripping of cluster galaxies X-ray emission from clusters of galaxies ]. (Oct., 2013) 3511–3525 astro-ph/9811117 arXiv:astro-ph/0411561 . Group-Cluster Merging and the Formation of Starburst Galaxies ,[ ,[ Nature (Nov., 2014) 148 434 , MNRAS , 795 0903.3818 L21–L25 1007–1016. medium hydrogen in Virgo Cluster spirals. 3:1003–1017 Surface density profiles of the gas [ ApJ counterparts as high-density regions of intragroup HI rings and arcs in the M96 group when, how, and why? effects in Atomic Gas (VIVA). I. The Atlas and the H I Properties Spiral Galaxies in Coma L15–L19 MNRAS Their Evolution Virgo Cluster Spiral NGC 4522 formation, mass distribution and morphology of galaxies Giant H I Anomaly in the NGC 3256 GROUP of a giant HI tail in the galaxy group HCG 44 evolutionary mechanisms in galaxy clusters: neutral(Apr., atomic 2010) hydrogen 1175–1192 in Abell1367 [28] L. L. Cowie and A. Songaila, [27] P. E. J. Nulsen, [29] V. Cayatte, C. Kotanyi, C. Balkowski and J. H. van Gorkom, [31] M.-S. Shin and M. Ruszkowski, [30] Y. M. Bahé and I. G. McCarthy, [26] S. E. Schneider, G. Helou, E. E. Salpeter and Y. Terzian, [33] W. Kapferer, C. Sluka, S. Schindler, C. Ferrari and B. Ziegler, [16] A. Chung, J. H. van Gorkom, J. D. P. Kenney, H. Crowl and B. Vollmer, [18] C. L. Sarazin, [21] H. Bravo-Alfaro, V. Cayatte, J. H. van Gorkom and C. Balkowski, [24] K. Bekki, [25] K. Bekki, B. S. Koribalski, S. D. Ryder and W. J. Couch, [32] S. Tonnesen and J. Stone, [19] J. E. Gunn and J. R. Gott, III, [20] J. D. P. Kenney, J. H. van Gorkom and B. Vollmer, [23] T. Westmeier, B. S. Koribalski and R. Braun, The MeerKAT Fornax Survey [15] J. English, B. Koribalski, J. Bland-Hawthorn, K. C. Freeman and C. F. McCain, [17] P. Serra, B. Koribalski, P.-A. Duc, T. Oosterloo, R. M. McDermid, L. Michel-Dansac et al., [22] T. C. Scott, H. Bravo-Alfaro, E. Brinks, C. A. Caretta, L. Cortese, A. Boselli et al., PoS(MeerKAT2016)008 , , , , in An H I and P. Serra , 422 , HI Ω (Nov., 2013) , The H I mass MNRAS , 777 (Dec., 2011) 28 , (Dec., 2002) The COS-Halos 197 ApJ 337 , , ]. ]. ApJS , (1998) 267–316 (May, 2005) L30–L34 MNRAS 36 , 359 The evolution and star formation The HIPASS catalogue: Star formation in shocked cluster 1405.1033 Environmental dependence of the H I ,[ (Apr., 2016) 4393–4405 Formation in Disk Galaxies under Strong ARA&A ]. , 2 MNRAS ]. , ]. 457 (Sept., 2001) 1076–1094 , pp. 867–+, 2001. ]. Morphology, Environment, and the H I Mass 326 MNRAS 13 , Simulations of ram-pressure stripping in galaxy-cluster 1605.03304 arXiv:astro-ph/0411349 1604.05193 The Chandra Fornax Survey. I. The Cluster Environment ,[ ,[ ,[ MNRAS ]. 1408.3392 , ,[ HI in the Three Largest LEnticulars in the Ursa Major Cluster (Sept., 2014) L114–L118 ]. astro-ph/0406216 The H I extent and deficiency of spiral galaxies in the Virgo cluster 443 ,[ Star formation in ram pressure stripped galactic tails Significant Enhancement of H . (J. E. Hibbard, M. Rupen, & J. H. van Gorkom, ed.), vol. 240 of 1203.0308 (May, 2016) L33 ]. ]. ]. ,[ (June, 2016) A51 MNRAS , 822 (Mar., 2005) 215–226 591 ]. ]. ApJL 621 ]. , A&A (Nov., 2014) 3559–3570 , The Lyman Alpha Forest in the Spectra of QSOs astro-ph/0210170 ApJ , (Nov., 2005) 154–164 ,[ 444 (July, 1983) 881–908 633 1309.6317 88 ,[ astro-ph/0106376 astro-ph/9806286 1110.3431 1510.07050 astro-ph/0502257 641–656 [ Survey of Six Local Group Analogs.[ II. H I Properties of Group Galaxies [ Survey: Rationale, Design, and a Census59 of Circumgalactic Neutral Hydrogen of dwarf galaxies in the Fornax Cluster The large-scale distribution of neutral hydrogen in the Fornax region AJ ApJ Ram Pressure Astronomical Society of the Pacific Conference Series interactions [ Gas and Galaxy Evolution [ MNRAS (May, 2012) 1609–1624 spirals and their tails environmental effects on the HI mass function of galaxies Function mass function in the ALFALFA 70% catalogue function and velocity width function of void galaxies in the Arecibo Legacy Fast ALFA Survey [48] C. A. Scharf, D. R. Zurek and M. Bureau, [47] M. Waugh, M. J. Drinkwater, R. L. Webster, L. Staveley-Smith, V. A. Kilborn, D. G. Barnes et al., [43] D. J. Pisano, D. G. Barnes, L. Staveley-Smith, B. K. Gibson, V. A. Kilborn and K. C. Freeman, [49] R. Giovanelli and M. P. Haynes, [45] J. Tumlinson, C. Thom, J. K. Werk, J. X. Prochaska, T. M. Tripp, N. Katz et al., [46] M. J. Drinkwater, M. D. Gregg, B. A. Holman and M. J. I. Brown, [44] M. Rauch, [42] M. A. W. Verheijen and M. Zwaan, [36] B. Henderson and K. Bekki, [37] D. Steinhauser, S. Schindler and V. Springel, [39] C. M. Springob, M. P. Haynes and R. Giovanelli, [35] E. Roediger, M. Brüggen, M. S. Owers, H. Ebeling and M. Sun, The MeerKAT Fornax Survey [34] S. Tonnesen and G. L. Bryan, [38] M. A. Zwaan, M. J. Meyer, L. Staveley-Smith and R. L. Webster, [40] C. M. Moorman, M. S. Vogeley, F. Hoyle, D. C. Pan, M. P. Haynes and R. Giovanelli, [41] M. G. Jones, E. Papastergis, M. P. Haynes and R. Giovanelli, PoS(MeerKAT2016)008 , , D The , 3 376 , ]. , (May, P. Serra A&A The HI , , The 422 (Apr., 2009) project - X. ]. project - D The ATLAS 3 D project - XIII. 694 3 D (Oct., 2011) Cosmic evolution 3 MNRAS (June, 2016) 110 ApJ , (Apr., 2007) 213–224 , 417 Dying radio galaxies in ]. 824 (June, 2011) 940–967 169 The ATLAS (Nov., 2014) 3388–3407 1606.04905 The ATLAS The ACS Fornax Cluster astro-ph/9712293 ApJ The ATLAS 414 , MNRAS 444 Environmental Effects in ApJS , , (Dec., 2011) 1649–1667 . 1308.1676 418 MNRAS ,[ , MNRAS , (June, 2016) , [ MNRAS Cluster radio relics as a tracer of shock waves ]. ]. , (Apr., 1998) 395–409, [ ]. 14 (Aug., 1989) 367–418 332 ArXiv e-prints , (Nov., 2013) 34–70 98 1408.2531 1011.0567 A&A AJ ,[ , 436 ,[ , ]. Fermi Large Area Telescope Detection of Extended Gamma-Ray ´ c, T. Naab, T. Oosterloo, R. Morganti et al., MNRAS , ]. ]. astro-ph/0107390 ]. ,[ 1111.4241 (Feb., 2011) A148 ,[ Population studies in groups and clusters of galaxies. II - A catalog of galaxies in the ]. 526 ]. ]. ]. 0812.2922 (Nov., 2015) 3980–3998 ,[ 1107.0002 A&A ,[ 453 , 1401.3180 1102.4633 1604.08862 astro-ph/0702320 1105.2294 2012) 1835–1862 882–899 XXVI. H I discs in real and simulated fast and slow rotators 1435–1451 clusters Atomic and molecular gas in the merger galaxy NGC 1316 (Fornax A) and its environment central 3.5 deg of the Fornax Cluster of the large-scale structure formation Emission from the Radio Galaxy Fornax A Survey. I. Introduction to the Survey and Data Reduction Procedures [ Mass and morphology of H I in early-type galaxies as a function of environment [ Clusters: Modified Far-Infrared-Radio Relations within Virgo Cluster Galaxies (Sept., 2001) 837–852 MNRAS [ GALEX Arecibo SDSS Survey - VIII.content Final of data massive release. galaxies The effect of group environment on the gas impact of environment and mergers on the H I content of galaxies in hydrodynamic simulations Content of Galaxies in Groups and[ Clusters as Measured by ALFALFA [ project - IV. The molecular gas content of early-type galaxies On the origin of the molecular and ionized gas in early-type galaxies of the atomic and molecular gas contents of galaxies [60] H. C. Ferguson, [61] M. Murgia, P. Parma, K.-H. Mack, H. R. de Ruiter, R. Fanti, F. Govoni et al., [63] C. Horellou, J. H. Black, J. H. van Gorkom, F. Combes, J. M. van der Hulst and V.[64] Charmandaris, T. A. Ensslin, P. L. Biermann, U. Klein and S. Kohle, [58] P. Serra, L. Oser, D. Krajnovi [59] E. J. Murphy, J. D. P. Kenney, G. Helou, A. Chung and J. H. Howell, [62] The Fermi-LAT Collaboration, [55] L. M. Young, M. Bureau, T. A. Davis, F. Combes, R. M. McDermid, K. Alatalo et al., [52] M. Rafieferantsoa, R. Davé, D. Anglés-Alcázar, N. Katz, J. A. Kollmeier and B. D. Oppenheimer, [56] P. Serra, T. Oosterloo, R. Morganti, K. Alatalo, L. Blitz, M. Bois et al., [57] T. A. Davis, K. Alatalo, M. Sarzi, M. Bureau, L. M. Young, L. Blitz et al., [54] A. Jordán, J. P. Blakeslee, P. Côté, L. Ferrarese, L. Infante, S. Mei et al., The MeerKAT Fornax Survey [50] C. D. P. Lagos, C. M. Baugh, C. G. Lacey, A. J. Benson, H.-S. Kim and C. Power, [51] B. Catinella, D. Schiminovich, L. Cortese, S. Fabello, C. B. Hummels, S. M. Moran et al., [53] M. C. Odekon, R. A. Koopmann, M. P. Haynes, R. A. Finn, C. McGowan, A. Micula et al., PoS(MeerKAT2016)008 , ]. 83 ]. 813 , P. Serra ApJ The , (June, The (May, A&A , ApJL 378 (Aug., 2012) 440 , The Fornax , p. 221, Jan., 29 , 1008.4616 ]. 1210.4448 Tidal origin of NGC ,[ ,[ MNRAS MNRAS PASA Maps of the Cosmos , , , The Herschel Fornax , in The Herschel Fornax (June, 2014) 274–288 IAU Symposium ]. 441 1710.09947 _H I from the 40% ALFALFA (Jan., 2011) 4 Simulating cosmic rays in clusters . ,[ Ω 141 (Oct., 2001) 812–826 VLA observations of neutral hydrogen in AJ MNRAS , (Jan., 2013) 834–844 377 , ]. 1205.1919 428 ,[ ]. A&A Clusters of galaxies: observational properties of , ]. 15 The Small Scatter of the Baryonic Tully-Fisher MNRAS (Sept., 1990) 604–634 The H I deficiency of the Virgo cluster spirals , 1008.5107 (Feb., 2018) 1108–1115 ,[ ]. 100 1512.04543 (May, 2012) 54 474 AJ ]. ,[ , 20 ]. 1008.0031 ]. ]. ,[ The Galaxy Evolution Explorer - Early Data MNRAS , A&ARv , ]. 1602.02149 ,[ (Jan., 2016) L14 1403.0589 1510.02475 ,[ ,[ astro-ph/0611037 Overview on Spectral Line Source Finding and Visualisation (Nov., 2010) 1359–1374 816 ,[ ]. 723 Only the Lonely: H I Imaging of Void Galaxies 1206.6916 ApJL ,[ , ApJ (Dec., 2010) 1868–1881 , (Mar., 2016) 42 140 arXiv:astro-ph/0108223 1403.1705 [ Survey Cluster Survey - I. The bright galaxy sample 2014) 1571–1589 359–370 Hulst et al., AJ Arecibo Legacy Fast ALFA Survey. X. The H I Mass Function and Cluster Survey II: FIR properties of optically selected Fornax cluster galaxies [ (M. Colless, L. Staveley-Smith and R.2005. A. Stathakis, eds.), vol. 216 of Wide-field Infrared Survey Explorer (WISE): Mission Description and Initial On-orbit Performance Unveiling a Rich System of Faint Dwarf Galaxies in the Next Generation Fornax Survey Distribution of slow and fast rotators in the Fornax cluster Where is the neutral atomic gas in Hickson groups? the diffuse radio emission Relation of galaxies - I. Effects on2007) the 385–408 Sunyaev-Zel’dovich effect and the X-ray emission 1427A in the Fornax cluster Deep Survey with VST. I. The820 Extended and Diffuse Stellar Halo of NGC 1399 out to 192 kpc (Nov., 2015) L15 (Mar., 1980) 38–51. Virgo Cluster galaxies. I - The Atlas [80] K. Kreckel, E. Platen, M. A. Aragón-Calvo, J. H. van Gorkom, R. van de Weygaert, J. M. van der [72] J. I. Davies, S. Bianchi, M. Baes, A. Boselli, L. Ciesla, M. Clemens et al., [75] C. Martin and GALEX Team, [77] B. S. Koribalski, [78] P. Chamaraux, C. Balkowski and E. Gerard, [76] E. L. Wright, P. R. M. Eisenhardt, A. K. Mainzer, M. E. Ressler, R. M. Cutri, T. Jarrett et al., [67] F. Lelli, S. S. McGaugh and J. M. Schombert, [71] R. P. Muñoz, P. Eigenthaler, T. H. Puzia, M. A. Taylor, Y. Ordenes-Briceño, K. Alamo-Martínez et al., [73] C. Fuller, J. I. Davies, R. Auld, M. W. L. Smith, M. Baes, S. Bianchi et[74] al., N. Scott, R. L. Davies, R. C. W. Houghton, M. Cappellari, A. W. Graham and K. A. Pimbblet, [81] L. Verdes-Montenegro, M. S. Yun, B. A. Williams, W. K. Huchtmeier, A. Del Olmo and J. Perea, [66] L. Feretti, G. Giovannini, F. Govoni and M. Murgia, [68] A. M. Martin, E. Papastergis, R. Giovanelli, M. P. Haynes, C. M. Springob and S. Stierwalt, [69] K. Lee-Waddell, P. Serra, B. Koribalski, A. Venhola, E. Iodice, B. Catinella et al., [79] V. Cayatte, J. H. van Gorkom, C. Balkowski and C. Kotanyi, The MeerKAT Fornax Survey [65] C. Pfrommer, T. A. Enßlin, V. Springel, M. Jubelgas and K. Dolag, [70] E. Iodice, M. Capaccioli, A. Grado, L. Limatola, M. Spavone, N. R. Napolitano et al.,