Pos(HEASA 2016)018 , Fermi

PoS(HEASA 2016)018 , Fermi http://pos.sissa.it/ . For one of these objects, Fermi Gamma-ray Space Telescope ∗ [email protected] [email protected] [email protected] Speaker. NGC 1068, a starburst galaxyflow which driven by is the also active the nucleus iswe brightest a compare and likely this closest source case of Seyfert both to 2,jet the other a emission. radio possible and Other galactic galaxies explanations gamma-ray out- with spectra, including both and starburstNGC starburst 253, and activity Circinus, Seyfert and and characteristics, blazar-like NGC including 3256, NGC show 4945, and varying AGN-driven degrees outflow. of Given evidence the of existence starburst, of AGN various mini-jet at possible emission high mechanisms energies, operating we discuss prospectsHESS for and observations the of Cerenkov starburst/Seyfert Telescope galaxiesKM3NeT. Array with (CTA), as well as future neutrino telescopes such as A handful of non-blazar galaxies,served including to emit both gamma-rays Seyfert by and the starburst galaxies, have been ob- ∗ Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 4th Annual Conference on High Energy25-27 Astrophysics August, in 2016 Southern Africa Cape Town, South Africa Sergio Colafrancesco School of Physics, University of theE-mail: Witwatersrand, Johannesburg, South Africa School of Physics, University of theE-mail: Witwatersrand, Johannesburg, South Africa Nebiha Shafi School of Physics, University of theHartebeesthoek Witwatersrand, Radio Johannesburg, South Astronomy Observatory, Africa Krugersdorp 1740,E-mail: South Africa Andrew Chen Prospects for very high energy observationsStarburst/Seyfert of galaxies PoS(HEASA 2016)018 Andrew Chen 1 ) or external seed photons coming from the disk, broad-line SSC The current understanding of AGNs is that they are supermassive black holes at the center Blazars exhibit a non-thermal spectral energy distribution (SED) which spans from radio to In hadronic models, proton acceleration produces synchrotron, photo-hadronic and/or proton- Active galaxies comprise the majority of sources detected by space-borne gamma-ray observa- of the host galaxyelectromagnetic whose energy, emission when the is nearby poweredAGNs material are by accretes observed to the onto produce the conversion jets, black collimated ofWhen beams hole[10]. gravitational of the plasma A jet potential exhibiting fraction is bulk into of relativistic aligned motion. the with emission the and the line AGN of is sight, classified the as a Doppler blazar[11]. boosted radiationgamma-ray of with the two jet broad dominates peaks.emission The from low-energy peak high-energy is electrons thought interacting to withmodels, be the the produced magnetic high-energy by field synchrotron peak within the iselectrons jet. up-scatter produced In photons by leptonic produced inverse either Comptontrons through emission, (synchrotron synchrotron self-Compton where emission or the from those high-energy same elec- proton cascade emission. The broadlog-parabola high spectrum in energy gamma-rays[13]. hump yields a power law, broken power law, or 2. Gamma-Ray Emission Mechanisms 2.1 Jet emission region, cosmic microwave background, or other radiation backgrounds[12]. tories sensitive in the 20 MeV tofraction 300 GeV of energy sources band[1][2], as detected well by as20 accounting ground-based GeV for to imaging a 200 significant Cerenkov TeV telescope energythe band arrays vast (e.g., sensitive majority MAGIC, in of VERITAS, H.E.S.S.)[3][4]. gamma-ray the detected Itjet active is galactic emission[5]. known nuclei today (AGN) In that are the blazars casesteep powered by of spectrum their Fermi radio sources, quasars even (consideredgalaxies[7] non-blazar are to objects also be such most misaligned as likely blazars)[6] radio poweredincluding by and galaxies starburst jet and galaxies narrow-line emission. such Seyfert as Only 1 thought M82, a to NGC handful emit 4945, of gamma NGC extragalactic rays sources, through 253, interactionswith NGC of the 6814, cosmic and interstellar rays accelerated Circinus[8], gas in are and supernovadiffuse remnants low-energy emission photons. in the This Milky isboth Way[9]. known the as same One a mechanism interesting starburst that sourcecompare galaxy produces some detected and the AGN by a and Seyfert Fermi, starburst 2 NGC modelsintroduce galaxy, a 1068, which and third can is therefore alternative, plausibly an the fit emission AGN.marize the In through the spectrum AGN-driven this evidence galactic of paper for outflows. NGC we or We 1068 against brieflyincluding and AGN-driven sum- NGC galactic 4945, outflow NGC in 253, otherstarburst/Seyfert starburst/Seyfert and galaxies galaxies Circinus. with current We and then future exploreent gamma-ray the models and prospects of neutrino the for telescopes broadband observations under emission. of differ- VHE observations of Starburst/Seyfert galaxies 1. Introduction PoS(HEASA 2016)018 Andrew Chen Third Source Catalog (3FGL)[1] Fermi-LAT 2 330 GeV [19]. We examine whether the gamma-ray emission > th 70 MeV in the galaxy rest frame[8]. for 1-100 GeV. The H.E.S.S. collaboration reported an upper limit of E 1 ≥ − for s 2 1 − − s and showed that the broadband SED of NGC 1068 could derive from a leptonic 2 100 pc scale with a velocity of 100-200 km/s [14][15]. This outflow can induce − ∼ ph cm 9 − Fermi ph cm 10 12 × − ) 1 10 ± × Lenain et al. (2010) [20] first reported the detection of Seyfert 2 galaxies NGC 1068 and In some starburst/Seyfert galaxies (such as NGC 1068), sub-mm interferometry of molecu- NGC 1068 is the closest AGN, at a distance of 14.4 Mpc. Like many Seyfert 2 galaxies, a In galaxies undergoing active star formation, massive stars exhaust their nuclear fuel, collapse, 6 ( 76 . jet scenario. Interestingly, theirseed model photons are includes infrared an photons external dueby to inverse relativistic dust Compton electrons re-emission component at of whose absorbed a starlight few being tenths up-scattered of parsecs from the central source within the misaligned NGC 4945 by observed by Fermi is primarily due toand a the blazar-like AGN implications jet, of starburst different activity, or models some for other TeV origin, observations. 3.1 Jet emission hypothesis of 5 lar lines in the circumnuclearwhich disk extends to (CND) suggests theshocks existence in of the a CND, giant, which, AGN-driven inexceed outflow turn, that can in accelerate relativistic Supernova particleselectromagnetic remnants with bands (SNR) an [16][17]. efficiency and that could may Intral leave addition pions observational to created signatures primary by in collisions acceleratedambient different between protons electrons, may relativistic the produce protons decay a accelerated significant ofsion by gamma-ray can neu- emission. the be Such favored AGN as hadronic shocks the gamma-rayMeV. with dominant emis- At component lower of energies the leptonic gamma-ray processesbremsstrahlung spectrum can like at significantly inverse energies contribute Compton above to 100 (IC) the gamma-ray scatteringresponsible emission. for and IC Finally, non-thermal the and same bremsstrahlung electrons emission spiralingchrotron in emission interstellar magnetic in fields the radiate syn- radioare continuum. determined by In the energy this supplied picture, to the relativistic protons gamma-ray and and electrons radio at luminosities the3. shock. The case of NGC 1068 Seyfert 1-like spectrum with broadthe lines AGN unification is scenarios, revealed this when is evidence viewed thatand in the dust[18]. nucleus polarized is NGC light; obscured 1068 by according a is to is clumpy also torus a undergoing of gamma-ray gas active star emitter, formation with in a its flux central according region. to NGC the 1068 2.3 AGN-driven outflow models and undergo supernova explosion. The remnant producesproduce an high expanding shell energy whose cosmic shock rays front can throughthey interact diffusive shock with the acceleration. interstellar If medium of hadronsThe the are host main accelerated, galaxy neutral and produce pion charged andcharacteristic decay neutral pion pions. mode bump at yields two gamma rays producing hence a spectrum with a VHE observations of Starburst/Seyfert galaxies 2.2 Star formation PoS(HEASA 2016)018 ) 1 ∼ − ˙ M 100 pc with 400 km s Andrew Chen ∼ ∼ 100 pc spatial resolution[14][15]. − 10 ∼ 400 pc) outflow extending up to 3 − 50 ∼ r in several molecular line tracers probed by ALMA[14][15][27]. . Comparison of the kinetic energies associated with AGN activity 1 1 − − ergs 41 2 kpc region of NGC 1068 with 10 ∼ × r 5 ∼ 200 pc size which is noticeably off-centered relative to the AGN. a-Burillo et al. (2014)[15] estimated the molecular outflow rate in the CND, kin × L , assuming a multi-conical outflow geometry, with a corresponding kinetic luminosity 1 − yr On the other hand, this AGN-driven outflow in the CND can induce shocks that lead to the Yoast-Hull et al. (2014)[21] and Eichmann & Becker Tjus (2016)[22] have developed mod- Radio continuum observations have spatially resolved a number of nuclear structures - a Perhaps the most interesting result of these high resolution observations is the gas kinematics GarcÃ

M acceleration of cosmic rays (e.g. [30][31]).an Several intriguing molecular evidence line for abundance a ratio studies connection provide between the CND and cosmic rays. Chemical analysis of and nuclear starburst showsIn that fact AGN either activity the is radiomolecular the outflow jet (e.g. and/or more [15][29]). AGN likely radiation source pressure powering are the found outflow. to be capable of driving the 63 outflow of els for the gamma-ray emissionproduced and in broadband supernovae with SED interstellar from matter interaction andstar radiation of formation from high starburst rate. energy galaxies based cosmic on They rays gamma-ray their have spectrum shown of that other starburst diffuseNGC galaxies cosmic 1068. are ray unable The models to star which explain formationleast the successfully a rate gamma-ray few fit of to emission several NGC the orders of 1068 of magnitudeing would in the need order to parameters to fit for be the fitting observed higher gamma-ray theemission by flux. gamma-ray compared a Moreover, flux to us- factor significantly the overestimates of observed the from radio radio flux. at synchrotron 3.3 Giant AGN-driven outflow 2 kpc starburst disk,(CND)[23][24][25], and a a kpc-scale sub-arcsecond jet-cloud radiosub-mm interaction jet, (around interferometry 20 observations a pc)[26]. have pc-scale More illuminatedgas jet recently, in the surrounded the distribution central by and kinematics a molecular circumnuclear disk VHE observations of Starburst/Seyfert galaxies jet, which provides the bulk ofCompton the gamma-ray (SSC) emission component. compared to This a indirectcomparable negligible synchrotron dependence obscured self- on Seyfert 2 active star galaxiesof formation have NGC may gamma-ray 1068. explain luminosity why upper limits lower than that 3.2 Starburst hypothesis The ALMA CO (6-5) mapring of fully 350 resolved the CND and revealed a highly-structured asymmetric revealing evidence of a giant nuclear ( a velocity of 100 -Gallimore 200 et km al. s (2016)[28] furtherwith detected a a sign higher velocity of CO non-circularAGN (6 rotation accretion -5) that disk. emission is The ( consistent tightjet, spatial with correlation a and between bipolar the the outflow molecular AGN along ionizedThese outflow, the gas observations strongly outflow, axis also the suggests of radio provide that the strong theobscuring support torus. molecular for outflow the is dynamic AGN-driven[27]. disk-wind scenario for the AGN PoS(HEASA 2016)018 Andrew Chen -rays at both GeV and TeV energies γ 9 Mpc) that exhibits both starburst and . observations may be able to discriminate 3 ∼ 10 times lower than observed. The evidence for Fermi 4 − 9 Mpc) prototype starburst galaxy. It is hosts several 4 . 3 ≈ gamma-ray data from 3FGL[1] and the H.E.S.S. upper ∼ 2 Mpc) is one of the most extensively studied nearby galax- . 4 ∼ Fermi-LAT -rays [8]. γ , we plot the 1 NGC 4945 is another nearby spiral galaxy (d We consider in this section a few more examples of starburst/Seyfert galaxies in order to assess NGC 253 is a well-studied nearby (d The Circinus spiral galaxy (d Note that using commonly assumed proton and electron acceleration efficiencies, AGN-driven In Figure galaxies ies, situated behind the intense foreground of[42] the surrounded Galactic by plane. a Circinus hosts circumnuclearlobes a starburst perpendicular Seyfert [43]. 2 to nucleus the Radio disk, observations ashas have also well shown been as bipolar detected kpc-scale with radio jet-like the structures Fermi-LAT [44]. [45]. Gamma-ray emission their observability with the futureNGC very 4945 high-energy and NGC observatories: 3256. these are NGC 253, Circinus, strong coupling between the molecularfrom medium molecular in line the survey CND abundances discussed andcies in to the the the outflow required previous shock-produced level. section CR could boost the efficien- 4. Prospects for CTA and other gamma-ray observations of starburst/Seyfert compact objects including a possible- AGN [35][36]. with NGC multiphase 253 structure is -burst also believed galaxy known to is to be one host of driven a the by[40][8][41]. superwind two the starburst starburst galaxies (e.g. observed in [37][38][39]). The star- Seyfert characteristics (e.g.[46]). It also harboursorthogonal a powerful to nuclear the wind forming disk a of conicalto the plume NGC galaxy, 253. believed to At be highbeen starburst-driven energies detected wind NGC in [47][48], 4945 that is is one similar of the few starburst/Seyfert systems which have outflows would produce a gamma-ray flux limit[19]. We compare these data toand three an models; AGN outflow-driven a model[29]. simple SSCand We also jet 100 show model, hours predicted a of thresholds starburst observation. model[22], forwhile CTA-South The both for starburst the 50 model jet fails modelslightly to unrealistic and fit parameters. the the observed AGN While gamma-ray outflow-drivenbetween continued spectrum, model the are two models able at to thescopes fit such lowest and as the H.E.S.S. highest data, and energies albeit CTA (seeis are with [29] correct. the for most A further promising H.E.S.S. details), avenue detection for TeV wouldable tele- clearly support to showing the reveal which the AGN model TeV outflow-driven spectrum model, in while detail. CTA will be VHE observations of Starburst/Seyfert galaxies ALMA full resolution molecularCND. line Their studies studies revealed significant show that chemicalactivity), and a difference a across high component of the cosmic shocked ray gas are ionization present rate in (possibly every subregion3.4 combined of with the Comparison CND[30][32][33]. of X-ray models for the gamma-ray emission of NGC 1068 PoS(HEASA 2016)018 = 2 α , 0 = 1 Andrew Chen α ; see also [34]). 5 -rays [53], have been observed [52]: they are both late stage mergers with large γ indicative of an AGN-like jet. Blue dotted curve: model from starbursts of Eichmann https://www.cta-observatory.org/science/cta-performance , 5 . 3 Black dashed: a simple SSC model with main parameters spectral index ) = break Γ ( NGC 3256 is one of the most luminous galaxies beyond the local group. The system is a In order to estimate the prospects of observations of a list of starburst/Seyfert galaxies with log , Figure 1: merger of two galaxies andtwo contains bright, two extended nuclei tidal separatednuclei tails have by been [51]. 850 observed by pc ALMA [49][50] Twobipolar – and molecular jet a southern and known outflows outflow a for that associated northern its is outflow withsimilarities believed suggested to between each to be NGC be driven of 3256 by part and the an ofbe Arp AGN a two detected 220, starburst-driven in superwind GeV the [52]. first ultra-luminous Some infrared galaxy (ULIRG) to CTA and other gamma-ray observatories, weaccording first to calculate the the total procedure energy listedstarburst, budget and below. of AGN each We outflow-driven galaxy then emission) by scale energy the budget three and NGC distance 1068 and model we compare spectra the (jet, 3 infrared luminosities; outflows from both ofthe the two nuclei two with merger less nuclei than are 1rotational present kpc axes separation (e.g, [55]. still [54][52]); have and their own nuclear gas disks with misaligned and J. Becker Tjus (2016; seetheir their Fig. Fig. 2 7)[22]. magenta Magenta curve, solid model-1,the curve: dagger AGN model outflow)[29]. symbol from is Black the Lamastra dots H.E.S.S. et areby upper al. Fermi-LAT the limit[19]. data (2016; green from The see curves CTA-South 3FGL[1] sensitivity ( and for 50 and 100 hours is shown VHE observations of Starburst/Seyfert galaxies PoS(HEASA 2016)018 , p (4.1) (4.2) is the ) E ( τ Andrew Chen where ) is the volume of the E ( V τ ) E ( Q π ) = , E dE ( 4 51 N c E 2 π ) V ν π m cr E ), the outflow model would be difficult to ε ( − 2 0 2 π π is the supernova rate, = q E ν p 6 EdE min ∞ ) E E Z ( 2 Q max ergs, the typical energy from a supernova explosion. In an ) = min E γ E 51 E Z ( γ q such that p − 1 is 10 E = ) the SSC model fits the Fermi-LAT data, while the starburst model would ∝ 2 ) 51 E E ( Q is the particle acceleration efficiency, cr ε In the case of Circinus, the starburst model can reproduce quite well the GeV Fermi-LAT data In NGC 4945 (Fig. We emphasize that the comparisons between the gamma-ray data and the simple scaled NGC We notice that, in the case of NGC 253 (Fig. In order to get a rough estimate of the energy budget available to each galaxy, we use a simple including the spectral curvature at GeV energies, but with a steep high-energy spectrum which where starburst region, and have to be refined along thespectral lines of curvature. those The used for AGN NGC outflow-drivena 253 model quite [41] is flat in subdominant order spectrum at to at be GeVSSC TeV consistent energies model energies with would but that the lie provides lies near well the abovewould edge the be of the more nominal nominal difficult CTA CTA to sensitivity sensitivity detect. limits. limits while The the starburst model reconcile with the observed Fermi andCTA HESS would combined be spectrum. able More to preciseHESS rule observations spectrum with out is certain roughly outflow consistent scenarioscan with with also the greater fit SSC confidence. the jet gamma-ray model, The data and well; Fermi more see and detailed [41] for starburst three models examples. 1068 models as applied towe other have galaxies not should made be anycharacteristics. understood attempt to to have predict large the uncertainties, spectrum since of each source based on its own physical equilibrium condition the particle spectrumloss life then time becomes (due tofunction radiative from and the collisional proton spectrum losses). andproduction, using Adopting we the [56] calculate approach to the of calculate gamma-ray [57] emissivity the to from get pion the the source starburst/Seyfert cross sources sections as for pion 4.2 Results pion emission model based on the followingequilibrium basic assumptions: for uniform ISM particle particle distributions, injection(ignoring and escape), losses a due power only law to cosmic cosmic ray ray proton interactions injection spectrum with with the spectral ISM index of VHE observations of Starburst/Seyfert galaxies resulting spectra with the sensitivity oftrum of CTA. Note each source that based we on have itsof not own physical the attempted characteristics, to NGC but predict rather 1068 performed the model acomparisons spec- simple made spectra scaling below based should on be understood the to calculated have large total uncertainties. energy4.1 budget. Energy budget Consequently, calculation the and supernovae as the assumedfunction drivers spectrum of cosmic ray acceleration. Therefore, we adopt a source PoS(HEASA 2016)018 1 − s 2 − Andrew Chen ph cm 10 − 10 × 47 . ). The other two models here consid- 3 7 20 PeV. In NGC 1068, photo-hadronic cooling dominates proton- ≈ but for NGC 4945 and NGC 253. The HESS data for NGC 253 from [41] are ) has unfortunately only a Fermi upper limit of 3 1 3 100 GeV, which is not able to constrain the models. No publicly available TeV < E < Same as Fig. NGC 3256 (Fig. Any hadronic interactions which produce gamma rays through neutral pion decay will also ered (e.g., the SSC and theCTA AGN sensitivity outflow-driven limits. models) predict spectra that lie above the nominal proton by a factorcould of become (25-100). significant. At While lowernot past energies, sensitive and enough and current to in detectors detect otherKM3NeT such the may galaxies, neutrino as be proton-proton emission ANTARES sensitive and from enough. cooling these IceCube For a galaxies, are more future detailed detectors discussion such see as [29]. could make it more difficult to detect at CTA energies (Fig. produce neutrinos through charged pion decay. Detection offert neutrino galaxy emission would from therefore a starburst/Sey- provide conclusivecosmic-ray evidence protons of with hadron interstellar acceleration matter and and interactions radiation.getic of than The neutrinos the are initial a cosmic-ray factor protons, ofacceleration meaning 20 of that less detection protons ener- of up 1 to PeV neutrinos would indicate shown as blue squares. 5. Prospects for neutrino observations of starburst/Seyfert galaxies Figure 2: for 1 GeV upper limit exists for this source. VHE observations of Starburst/Seyfert galaxies PoS(HEASA 2016)018 Andrew Chen 3 arcmin for . https://www.cta- 8 but for Circinus galaxy and NGC 3256. 1 ; see also [34]). Same as Fig. Figure 3: Our group is in the process of pursuing a number of lines of enquiry. We are investigating We are also beginning an optical observing campaign of starburst/Seyfert galaxies including NGC 1068 is an interesting case of a gamma-ray emitting AGN that exhibits characteris- 3 TeV would also help distinguish between jet, starburst and outflow activity ( & observatory.org/science/cta-performance jet models which incorporateemission an of external absorbed Compton starlight component alongin with the this lines seed paper. of photons [20] We from todetectable are dust complement by also re- the CTA investigating under simple these different SSC andmodels emission model and other scenarios, used progressing starting starburst/Seyfert to with galaxies models simple tailored which to scaling may each of be starburst/Seyfert. NGC 1068 these galaxies with the South Africanline Large Telescope ratio (SALT). Observations have of been the used OVIIIemission to from to the OVII Fermi distinguish bubbles within between the supernova Milkyline Way[58]; ratios and our to observations AGN will distinguish use between models this jet, of and starburst,other other and the starburst/Seyferts. AGN-driven outflow gamma-ray models for NGC 1068 and E tics of a misalignedservations jet, in starburst the 100 activity,gamma-ray and GeV emission to AGN-driven from both outflow. TeV NGC spectral 1068NGC and range We other 253, have are starburst/Seyfert galaxies Circinus, argued the such and as key that NGCa NGC to ob- 4945, 3256. breakthrough, disentangling the while Ongoing source CTA observationsrange is of by and the Fermi ideally definitively and suited resolving H.E.S.S. to the may measuring lead ambiguity. the to spectrum The in CTA spatial the resolution relevant of energy 6. Discussion and Future Work VHE observations of Starburst/Seyfert galaxies PoS(HEASA 2016)018 , ]. (Aug., ApJ , The (Oct., (Sept., Fermi 755 Fermi An updated , Andrew Chen The major 558 720 GeV ApJ , ApJ A&A ]. , 1501.02003 , ,[ 1409.5594 (Oct., 2005) 465–472 ,[ (June, 2015) 23 441 218 ]. A&A , ApJS , 9 (Jan., 2016) 76–94 ]. 72 0911.3485 ,[ ]. ]. ]. 1501.06054 -ray sources and their variability in pointing mode γ ,[ . Astroparticle Physics 1310.4029 , 1206.1346 ,[ ,[ (Dec., 2009) L142–L147 ´ c, S. Ansoldi, L. A. Antonelli, P. Antoranz, A. Babic, P. Bangale et al., Observations of selected AGN with HESS 707 (Sept., 2015) 14 astro-ph/0507207 [ 810 ApJ 2012) 164 Radio-Loud Narrow-Line Seyfert 1 as a New Class of Gamma-Ray Active Galactic Nuclei 2013) A137 et al., upgrade of the MAGIC telescopes, PartCrab II: Nebula A performance study using observations of the Third Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope Large Area Telescope Observations of Misaligned Active2010) Galactic 912–922 Nuclei Observations of Star-forming Galaxies with the Fermi Large Area Telescope Large Area Telescope Third Source Catalog list of AGILE bright Another avenue of investigation involves neutrino observations. Observed neutrino flux would We thank A. Lamastra and co-authors for private communication of the details of the AGN [7] A. A. Abdo, M. Ackermann, M. Ajello, L. Baldini, J. Ballet, G. Barbiellini et al., [5] M. Ackermann, M. Ajello, W. B. Atwood, L. Baldini, J. Ballet, G. Barbiellini et al., [8] M. Ackermann, M. 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