sign in sign up
<<
Home , Active galactic nucleus, Arp 220

PoS(11th EVN Symposium)002 http://pos.sissa.it/ 150 pc of the Arp 299-A (D=45 Mpc), showing ∼ † ∗ [email protected] Speaker. Based on results obtained with the European VLBI Network (EVN). Luminous and Ultra-Luminous (U/LIRGs) aremal also strong (free-free) emitters and of non-thermal both ther- (mainly )unlike optical radio and emission. infra-red This observations, is radioU/LIRGs, is very which not handy allows obscured since, by a the directgalaxies. ubiquitous view dust of present the in ongoingIn activity this inside talk, those I prolific present -forming factory some in selected a results nearby on LIRG, Arp whatprolific 299. is Namely, probably factory I in the show the most (i) central spectacular the impressive supernova discovery of an extremely that essentially all core-collapse supernovae explodedetection in and precise the location central of 150 the pcthe long-sought of compact AGN sources the in in galaxy, Arp Arp (ii) 299-A, 299-A. the andlowing A (iii) URL: movie the http://www.iaa.es/ summarizing monitoring torres/research/arp299a.html. those of findings All can thosevery-high be results angular found resolution demonstrate in studies that the of fol- nearby U/LIRGssion are of of both high local relevance and for high-z the starbursting comprehen- piece galaxies, and of that such Arp studies. 299 stands itself as a fundamental ∗ † Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. c

11th European VLBI Network Symposium &October Users 9-12, Meeting, 2012 Bordeaux, France Miguel Pérez-Torres IAA-CSIC, Glorieta de la Astronomía s/n,E-mail: 18008 Granada, Spain Arp 299: The show must go on! PoS(11th EVN Symposium)002 ), ]) α − 11 (1.2) (1.1) m ]. 3 Miguel Pérez-Torres has taken place in Lu- z is proportional to m is the minimum mass of ! α α ]: SN 6 − − ]). 1 2 u 1 u m − )[ is the power-law coefficient of the m m 14 yr ], as their star-formation rates (SFR) α − − FIR 7 . Fortunately, radio is not affected by

, L α α 1 − − M − 2 l 1 SN  yr CCSN m m 0.05 mJy) radio searches, which proved that r

≤

]; IC 883 [ L 2  FIR , 11 2 1 2 L 10 10 − −  α α 2 .  17 explode as core-collapse supernovae (CCSNe), the observed ≈ SFR ) can be used as a direct measurement of the SFR in galaxies,

]; Arp 299 [ = 9 SFR 8 M CCSN r CCSN > ∼ r 05 arcsec), high-sensitivity ( . 0 ≤ is the constant rate in M are the lower and upper mass limits of the stars, and u m SFR Thus, starburst activity in the circumnuclear regions of LIRGs ensures both the presence of a A large fraction of the massive star-formation at both low- and high- However, the direct detection of CCSNe in the extreme densities of the central few hundred While the compact, centrally located radio emission in U/LIRGs might be generated by a and l where high number of massive starsto and occur. a Those dense SNe surrounding can medium, beangular so detected, resolution bright even ( in radio the SNe innermost are regions expected of U/LIRGs, by means of high are formidable in comparison with thosemodels in to field bursts galaxies. of Indeed, age by 10–100obtain applying Myr, the evolutionary and SFR stellar adopting as a a standard function initial of mass its function far-infrared (IMF), one ( can initial mass function (which states that the number of stars with mass they can unveil nuclear starburststhe and local detect Universe (e.g. individual radio supernovae [ up to large distances in pc of U/LIRGs is,suffers as very significant pointed out inat earlier, those best regions, extremely yield which difficult contain only since large a emission amounts lower of in limit dust, the to and the visual can true band value of Arp 299: The show must go on! 1. Introduction minous and Ultra-luminous Infrared Galaxies (U/LIRGs) [ m that yield supernovae. point-like source, i.e.radio an active supernovae galactic (RSNe) nucleus and/orcircumnuclear (AGN), supernova regions or remnants of by (SNRs), U/LIRGs the therestars it combined more is is effect massive an than well of ongoing M multiple established burst that of (massive) in star the formation. Since rate at which those starsand die may ( provide unique information about thesimplicity IMF we of assume the a high-mass constant stars. star-formation In rate fact, for if for a the starburst, sake it of can be shown that (e.g. [ dust absorption. Moreover, significant radio emission frommonuclear CCSNe SNe–as is the expected–as interaction opposed of to the ther- SNto ejecta a with high-energy the density circumstellar shell, medium which (CSM)amplify is gives the Rayleigh-Taylor rise unstable existing and magnetic drives field turbulent in motionselectrons, the that thus presupernova enhancing wind, the and emission efficiently of accelerate synchrotron relativistic radiation at radio wavelengths [ PoS(11th EVN Symposium)002 40) and the lack − Miguel Pérez-Torres 34 ∼ ] and references therein). ], one of which (A0) was 8 V the nuclear region of Arp 13 A ] and Figure 1-left). We found that the 10 ), the implied CCSN rate for the whole Arp ([

] and Fig. 1-right). A1, the brightest compact L 11 12 3 10 × 5 . 6 ≈ IR L 11.5. An active starburst in Arp 299 is indicated by the high fre- > )

/L FIR 1.8 SN/yr. Since about 50% of its total infrared emission comes from Arp 299-A, ≈ The dusty nuclear regions of luminous infra-red galaxies are heated by either an intense burst The merging system Arp 299 (D=44.8 Mpc) is the most in the nearby In 2008, we used the eEVN at 5.0 GHz to image the central region of Arp 299-A at high Optical and near-infrared observations are likely to miss a significant fraction of CCSNe in evidence for foreground (H II) absorbers radio of the compact objectsfrom in the Arp 299-A explosion were of typical type of IIP,very normal IIb well RSNe, and suited which IIL target result SNe. to eventually All determine these the results complete confirmed CCSN that2.2 rate Arp in Cohabitation 299-A a of was local starburst a LIRG. and AGN in Arp 299-A, a candidate, and of massive star formation, ortangling an the active galactic contribution nucleus of (AGN), eachdirect or of imaging a of those combination the putative of innermost dust-heating both. fewhigh-angular pc agents Disen- resolution can is only observations. a be Hence, challenging accomplished atunveil after task, the radio the and supernova wavelengths, factory successful using in very observations Arp that 299-A,cies, allowed we in proposed us the further to EVN hope observations ofcontemporaneous at unveiling EVN two the frequen- observations on nature Arp of 299-Acovery the showed of yet already the another discovered remarkable long-sought objects. result: AGN the The in dis- Arp 1.7 299-A and ([ 5.0 GHz source in Arp 299-A in ourThe 5.0 1.7 GHz GHz EVN EVN observations, image wasA5 showed also (Figure also the 1-right). diffuse, brightest low-surface The source brightness morphology, atemission radio emission 1.7 of luminosity, from the GHz. spectral A1–A5 A1 index region towards is and in ratio(LLAGN). perfect Since of agreement Arp radio-to-X-ray with expectations 299-A from had a longLLAGN low-luminous AGN been in thought its of central as regionstarburst a and and pure cohabitating AGN starburst, phenomena with our may a finding be recent of frequently burst a associated of in buried, mergers. star-formation, suggests that 50 Mpc, with Log(L resolution and with high sensitivity. These observations showed that Arp 299: The show must go on! 2. Arp 299 rocks! quency of recent optically discovered supernovaeSN in 1998T, this SN galaxy, 1999D, including SN SN 2005U, 1992bu, SNBased SN 2010O, on and 1993G, SN its 2010P infrared (see e.g. luminosity [ ( of the necessary angular resolution.resolution, high Therefore, sensitivity are radio the observations onlying of promising directly Arp way of its 299-A detecting CCSN at new rate high CCSNe,during and and 2002 angular SFR. thus and measur- 2003 Very Long resulted in Baselineidentified the Array as detection (VLBA) a of observations young five SN. carried compact sources out [ 2.1 An extremely prolific supernova factory in Arp 299-A unveiled with the EVN 299-A hosts an extremely prolific supernova factory 299 system is this makes of it an obvious target for searching recently exploded CCSNe. the innermost regions of Arp 299-A due to high values of extinction ( PoS(11th EVN Symposium)002 0 250 200 150 300 200 100 350 300 250 200 150 350 300 -300 A5 -20 -20 A5 -200 Blow-ups of the 7 June 2009 A1c 12 June 2009 -10 -10 Miguel Pérez-Torres -100 Jet component Jet components A1b 0 0 0 A1 A1 MilliARC SEC Contour maps drawn at five MilliARC SEC MilliARC SEC 100 A0 10 10 AGN core 200 20 20 300 1 pc 10 pc 1 pc 5.0 GHz EVN 5.0 GHz EVN 12 June 2009 1.7 GHz EVN Middle and bottom right: 0 50 5 0 5 0

20 15 10 -5 20 15 10 -5 200 150 100 -50

-100 -150 -200 -10 -15 -20 -10 -15 -20 MilliARC SEC MilliARC SEC MilliARC MilliARC SEC MilliARC Middle and bottom left: 4 5.0 GHz full EVN image of the central 150 region Top right: 5 GHz VLA archival observations of Arp 299 on 24 October 2000, displaying the five Top left: times the r.m.s. noise of our 5galaxy GHz Arp eEVN 299-A observations of on the 8 centralcompact, April 500 non-thermal 2008 emitting years and sources. of 5 the To guide luminous December theonly infrared 2008, reader’s at eye, revealing we the a show 5 large in December population cyanof the of 2008 components the relatively epoch. detected bright, luminous infraredemitting galaxy sources, mostly Arp identified 299-A, with younginner displaying RSNe 8 a and parsec SNRs. large of number themorphology, nuclear of spectral region index bright, of and compact, Arp luminositytypical 299-A, non-thermal of of as the AGNs. imaged A1–A5 Contours with are region drawn the are at full clear 5 EVN evidence and of at 10 times a 1.7 the core-jet and off-source structure, 5.0 r.m.s. GHz. noise. The brightest knots of radio emission in this merging galaxy. Figure 1: Arp 299: The show must go on! PoS(11th EVN Symposium)002 ]. 5 [ 0 . 1 150 pc. − r ∼ ∝ 2.5 yr) of 26 sn ∼ Σ Miguel Pérez-Torres 0.80 SN/yr, indicating > ∼ ] and Fig. 1). The properties of ] in Arp 299-C’ (see Fig. 1-left). 2 4 5 ]. If confirmed, A6 would be, together with the microquasar 2 100 pc of Arp 220 and Arp 299-A to show evidence for the , ∼ 150 pc of the galaxy Arp 299-A (D=45 Mpc) and the monitoring 12 ∼ ]. It is also remarkable that this RSN exploded at a mere (deprojected) ], one of the first extragalactic to be confirmed ever. 12 1 ], which is detectable at 5.0 GHz more than 8 yr after its discovery, but is 8 Here, I have presented some of the results obtained by my team on the interacting system More recently, we presented the first 5.0 GHz radio light-curve (spanning There is also growing evidence that A6 is a microquasar, based on its appearance and disap- It appears that foreground absorbers, i.e., H II regions, are responsible for the low-frequency Arp 299, making usesupernova factory of in the the central EVN, including the impressive discovery of an extremely prolific compact components in theall nuclear detected starburst objects of are Arp consistentobtained 299-A with for them ([ the first being time a a mixed directthat estimate population the of of CCSN bulk CCSNe rate of in and the Arp SNRs. currentWe 299-A have of star We also formation used in the Arp VLBI 299-Afor data is on the taking Arp first place 299-A, time in together the with theWe radial that innermost have on distribution found Arp of that 220 supernovae the andThis in surface M result the 82 density to central gives of probe regions support SNe of to followssupermassive starburst a theoretical black galaxies. power-law work holes, with that and radius, predictsAGN has and the important starbursts formation in implications of LIRGs. for nuclear understanding disks the around co-evolution of 3. Summary of a large number oflong-sought very compact AGN radio in sources Arp in 299-A.universe it, In have or addition, allowed the us VLBI detection to observations and estimateVLBI of precise the distant observations location energetics U/LIRGs of of in in the the magnetic the fields central existence and local of particles. nuclear We disks also in used and them, starbursts which in U/LIRGs. is aRecently, relevant we result for have detected models of theThis co-evolution radio SN of emission AGN was of discovered SN at 2010P [ IR wavelengths, and it took more than a year to show up bright in undetected at 1.7 GHz [ distance of two from thethe putative closest AGN to in a Arp central 299-A,accreting supermassive which models black makes in hole this ever the supernova detected. central onevery regions of This massive, of result supernova galaxies, progenitor may since stars also it so becould close is relevant explain to not to the an easy AGN. low-luminosity to While explain ofshed seemingly the large the contradictory, existence amounts this AGN of of we mechanical see energycreasing into in its their Arp temperature, surrounding those 299-A. medium, massive In therebyblack stars significantly fact, hole, would in- which since hinder could massive the in stars turn result of in material a to less2.3 the powerful central AGN The than nature usual. of the compact sources in Arp 299-A and their radial distribution pearance in our 5.0 GHz images [ Arp 299: The show must go on! candidates in Arp 220 [ absorption of the synchrotron radionificant emission number at of frequencies sources. around The and mostas remarkable below one 1.7 a is GHz, young likely for component RSN A0, a by previously sig- identified [ PoS(11th EVN Symposium)002 539 ApJ , A&A (1998) 189 , 36 (1982) 302 (2009) L17 Miguel Pérez-Torres ARA&A 259 The Astronomer’s 507 , , (2011) 95 An extremely prolific ApJ The Arp 299 show must go A&A , , 740 The nuclear starburst in ApJ , Evidence of nuclear disks in starburst galaxies (2012) L5 (2009) 1641 540 399 6 A&A , A Supernova Factory in the Merger System Arp 299 MNRAS , (2007) 314 659 (2011) A35 ApJ , Star Formation in Galaxies Along the Hubble Sequence 528 The radio and X-ray emission from type II supernovae Radio detection of the near-IR discovered supernova 2010P (2012) 1 A&A , Radio monitoring of NGC 7469: late-time radio evolution of SN 2000ft and the 4432 Evolution of the dusty infrared luminosity function from z = 0 to z = 2.3 using observations (2004) 186 circumnuclear starburst in NGC 7469 The Radio Spectra of the CompactSupernova Sources Remnants in Arp 220: A Mixed Population of Supernovae and Mattila, S., 611 supernova factory in the buried nucleus of the IC 694 C. N. A., from Spitzer Telegram from their radial distribution of supernovae & Ryder, S. D., Resolution of the Compact Radio Continuum Sources in Arp220 Arp 299-A: from the 5.0 GHz(2012) VLBI A134 radio light-curves to its core-collapse supernova rate I am grateful to the other members of the Arp 299 team (Antxon Alberdi, Marco Bondi, RubÃl’n [7] Magnelli, B., Elbaz, D., Chary, R. R., Dickinson, M., Le Borgne, D., Frayer, D. T., & Willmer, [8] Neff, S. G., Ulvestad, J. S., & Teng, S. H., [9] Parra, R., Conway, J. E., Diamond, P. J., Thrall, H., Lonsdale, C. J., Lonsdale, C. J., & Smith, H. E., [6] Kennicutt, R. C., Jr., [5] Herrero-Illana, R., Pérez-Torres, M. Á., & Alberdi, A., [4] Herrero-Illana, R., Romero-Canizales, C., Pérez-Torres, M. A., Alberdi, A., Kankare, E., Mattila, S., [2] Bondi, M., Pérez-Torres, M. A., Herrero-Illana, R., & Alberdi, A., [1] Batejat, F., Conway, J. E., Hurley, R., Parra, R., Diamond, P. J., Lonsdale, C. J., & Lonsdale, C. J., [3] Chevalier, R. A., [10] Pérez-Torres, M. A., Romero-Cañizales, C., Alberdi, A., & Polatidis, A., [11] Pérez-Torres, M. A., Alberdi, A., Colina, L., Torrelles, J. M., Panagia, N., Wilson, A., Kankare, E., & Herrero-Illana, and Cristina Romero-Cañizales) for their helpacknowledge during different financial stages of support this project. from Iprogramme. the warmly This organizers research of has the benefittedMINECO) from 11th through financial grants EVN support AYA 2009-13036-C02-01 Symposium by and the AYA 2012-38491- throughfunds, C02-02, Spanish as the cofunded Government well with (MICINN RadioNet3 as FEDER support and by126. the Andalusian The Autonomic Government European through VLBI grantsastronomy P08-TIC-4075 Network and institutes is TIC- funded a by joint their facility national research of councils. European, Chinese, South AfricanReferences and other radio Arp 299: The show must go on! radio. In Arp 299-B, we areunclear. monitoring All the those evolution results of show a that brighthigh very-high radio relevance angular “burp”, for resolution whose the studies nature comprehension of isArp still nearby of U/LIRGs 299 both are an local of and extraordinary laboratory high-zon! starforming in galaxies, our and local make universe. of No doubt, Acknowledgments PoS(11th EVN Symposium)002 The (2012) A72 543 Miguel Pérez-Torres A&A , Serendipitous discovery of the (2011) 2688 (2010) L5 415 519 MNRAS e-MERLIN and VLBI observations of the luminous A&A , , 7 infrared galaxy IC 883: a nuclear starburst and an AGN candidate revealed long-sought in Arp 299-A core-collapse supernova rate in Arp 299 revisited [14] Romero-Cañizales, C., Pérez-Torres, M. A., et al., Arp 299: The show must go on! [12] Pérez-Torres, M. A., Alberdi, A., Romero-Cañizales, C., & Bondi, M., [13] Romero-Cañizales, C., Mattila, S., Alberdi, A., Pérez-Torres, M. A., Kankare, E., & Ryder, S. D.,