PoS(EXTRA-RADSUR2015)008 http://pos.sissa.it/ † ∗ [email protected] Speaker. On behalf of the Radio Galaxy Zoo science team. We present a description and earlyproject results for from visual Radio inspection Galaxy and Zoo, classificationare a of to web-based classify all-sky individual citizen radio radio science surveys. sourcesmorphologies) The (particularly as galaxies goals well with as of matching multiple the the lobes project continuum and/or radiocome emission complex from to the the host FIRST galaxy. and Radio images ATLASinfrared surveys, imaging while from matches WISE to and potential SWIRE. hostsmore The are than first performed 1 twelve with months million of classifications classificationconsensus of have by more yielded than the 60,000 volunteer sources. classifiers,expert science For the team. images accuracy Based with is on at comparableprimarily mid-infrared least a colors, to 75% the mixture visual hosts of inspection associated ellipticalprevious by with galaxies, studies. radio the QSOs, emission The and full are catalog LIRGs, ofpopulations which radio of is lobes host in and types their good as host agreementalso a galaxies with been will function measure an of the radio effective relative method morphologyradio for and detecting power. galaxies. extremely Radio rare Results Galaxy objects, Zoo frommatching such has the for as use project in HyMORs future are and large being giant continuumcitizen surveys used science such in as to EMU, projects train as such well automatic as as the algorithms establishing SKA. roles for for host ∗ † 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). (*) This conference has been organizedInternational with Cooperation, the Directorate support General of for the theZA14GR02 Ministry Country - of Promotion Mapping Foreign (Bilateral the Affairs Grant Universe and Agreement on the Pathway to SKA) School of Physics and Astronomy, University55455, of Minnesota, USA 116 Church St. SE,E-mail: Minneapolis, MN EXTRA-RADSUR2015 (*) 20–23 October 2015 Bologna, Italy Kyle W. Willett Radio Galaxy Zoo: host galaxiesmorphologies and for radio large surveys from visual inspection PoS(EXTRA-RADSUR2015)008 detections 7 10% of triple Kyle W. Willett ∼ 000 galaxies from the FIRST , ). 1 175 ∼ 2 30% of double sources. It is also limited by being trained for specific geometries; ∼ Visual inspection of radio images overlaid with optical/IR improves on simple positional Several automated methods (eg, nearest neighbor) exist to model radio morphologies with their One of the most powerful methods of exploring the evolution of structure in the Universe is To transform radio emission into physical measurements of individual galaxies, the radio emis- Simple positional matching of radio continuum to optical/IR data of the same field can miss of extragalactic radio sourceswithout expected. extensive astrophysical Associating training and radioWe present is emission the not with design limited and its to earlyproject host [2] the output that of professional can is Radio matching community be radio Galaxy alone. emission done Zoo to (RGZ), near-IR hosts a for web-based citizen science matching, and to dateamount has of been data used capable successfullytronomers of given with being the data expected processed from outputs will of many scale surveys surveys. such far as beyond However, EMU the [1], the with ability more of than professional 10 as- optical/IR counterparts. For example,assessing linear whether triple multi-component systems sources in are well-fit thegies by ATLAS [5]. variations survey on This are lobe-core-lobe method modeled morpholo- uses by aas Bayesian well prior to as constrain the thearrangement, likely apparent separation which bending between is components angle. thenthe A compared accuracy. likelihood to The ratio the algorithm result is has of used a expert to fairly visual identify high classification success the [6] rate, most but to probable mis-characterizes measure [3] and ATLAS [4] surveys. 2. Current methods for morphologically classifying radio emission sources and through the advent of large-scale radioa surveys. variety Galaxies of emit physical radio-wavelength radiation mechanisms,also through both associated thermal with and a non-thermal. wideintracluster range medium Radio-wavelength of for emission physical galaxy is processes, clusters,black including accretion holes, shocks and and and jets distributed interactions emission for co-located in galaxies with the with star central formation. supermassive sion must have a definitiveemission, association with typically a in galaxy optical as orgalaxy inferred infrared cannot from wavelengths. be either This determined stellar step or fromthus is quasar-like radio a critical continuum transformation since emission; from the measurementreference-independent redshift reference-dependent of values of values, the a such such distance as (and asastrophysics. power flux or density linear or size) angular enables size, the to majority ofsignificant the numbers of relevant sources inblack the holes, field. can Radio havebeyond emission, a the especially optical very from extent large jets of the angular associatedcomponents galaxy. with size which Furthermore, as can jets are be seen oftenthat arranged projected resolved a in into on radio multiple source either the discrete will linear sky havematching or core of that emission bent sources overlapping extends based fashion. with well on the positioneither galaxy There will be itself. is identify mis-identified So many or also while potential omit automated no radio-loud extended components galaxies, guarantee (see many Figure will Radio Galaxy Zoo 1. Motivation and science PoS(EXTRA-RADSUR2015)008 sources. 4 10 Kyle W. Willett > m emission from the µ 3 Example of a radio galaxy for which simple positional source matching fails. Red contours show Other automated algorithms are similarly limited to particular systems, typically double sources Expert visual classification can also be limited by high densities of background galaxies and The RGZ project is operated by the Zooniverse, the world’s largest citizen science platform the radio emission from the FIRST survey, while the background heatmap is 3.4 Figure 1: with a single optical/IR componenttional resources [7; and 8]. are limited Complex by radio the amount morphologies of require realistic more training datanon-linear computa- available. sources. However, the possibilitiestential for categories, complex including morphologies rare extend arrangements totails, such dozens etc. as of [9]. X-shaped, po- The ringed, primary narrow-hundreds impediment or or to thousands wide-angled this of is sources scale; [6], an but becomes individual impractical or for small the team surveys can with do this for and host to several dozen citizen science projects. In contrast to the original Galaxy Zoo project WISE survey. In this case,matching the radio components high to density their of nearestcan IR counterparts. sources identify However, even makes an four spurious untrained/lightly-trained large human associationsbottommost radio likely radio when component. components simply (Original as image a from [2], single Figure galaxy, 5e.) with its IRrare counterpart (but coincident extant) with systems either the withadditional many training. components or displaying non-linear structures require 3. RGZ interface Radio Galaxy Zoo PoS(EXTRA-RADSUR2015)008 Kyle W. Willett 3 arcmin. × 4 ). The radio data are pre-processed to identify only 2 , users are presented with a single panel in which radio data 1 . These are outlined as discrete components that the user can select by clicking on σ Screenshot of a randomly selected FIRST subject in the Radio Galaxy Zoo interface. The slider at http://radio.galaxyzoo.org When classifying on the website In a single classification, users select all radio emission they consider to be originating from 1 is overlaid on an infrared background (Figure [10; 11], in which users applied discretehas labels a from two-step a process hierarchical with decision tree, direct RGZ annotations classification on the image itself. strong components, using a medianpeaks absolute above deviation 3 statistic to selectthem; objects the full with radio flux image density by is the present user as as a they blue-tinted desire. layer, The the standard opacity image of size which shown can to be a user controlled is 3 Figure 2: the bottom controls the relative opacity betweenradio the component(s) overlaid and radio identify and the infrared location images. of Users the select infrared discrete counterpart(s), if present. a single radio galaxy by clickingcomponents, on they individual advance components in one the stepof image. and the After then selecting host the click galaxy radio counterpart”. on based If the there on image are multiple the to radio near-IRother sources identify in data. the radio the image, probable galaxies. users Users source can repeatrandomly-selected also both Once steps image have to the appears. identify the user option clicks Users of always ‘Done’, selecting have the “No the classifications IR option are to recorded discuss and the a data new, with other Radio Galaxy Zoo PoS(EXTRA-RADSUR2015)008 Kyle W. Willett m near-IR images in the µ . 2 . 5 ). We find that the majority of radio hosts have WISE 3 locations in which users identified the IR hosts. Informa- ) y , x ( Spitzer Space Telescope table, which locates an optical counterpart. If either catalog gives a successful cross- m (W1) band from the WISE survey [12]. The second set of 4,396 images focuses on a µ http://radiotalk.galaxyzoo.org Radio data from the catalog include measurements of angular size and position angle, number The project design and some early science results have been published in [2]. BelowSince we users in the RGZ project are matching the radio emission to near-IR images, this allows An image is retired from the system once a minimum number of individuals have classified it; Classifications for RGZ are stored in a Mongo database, with separate annotations linked to There are two sets of radio/IR data being processed in the initial phase of RGZ. The first 2 of components, peak and integrated flux densities.such as If distance, a physical redshift of size, the and galaxy peak is and known, integrated we luminosities. add data 5. Early science results describe three projects in progress using RGZ data. 5.1 Infrared colors of powerful radio galaxy hosts for a very large studytometry. of the Using global a properties preliminary ofexamined the set the host of (W1-W2) properties 33,127 and as sources (W2-W3) atection classified colors function in of by of the galaxies RGZ their WISE with IR all-sky in a catalog pho- its reliable (Figure first radio 12 association months, and de- we tion from the original WCSinto header J2000 on positions. the The FITS positioncatalog, cutouts of which is the locates then host the galaxy used nearestGalaxy is to object then translate in cross-matched the the to annotations W1 bothmatch, image the photometric AllWISE within and 3 spectroscopic information arcsec,the about and radio the source the in likely SDSS our host DR12 catalog. are added as metadata to that threshold is set to 5ambiguity users is for images the with location only of acomponents. single the radio Individual potential component classifications IR (in are host) this aggregated case,image and to the based at on only provide 20 the a majority users consensus vote. for classificationdiscrete This images radio is of done sources; with the by using multiple first only radio taking those theestimate classifications, most the a common kernel location arrangement density of of estimator the the is IRthan then counterpart. one applied radio This to galaxy is within repeated an if image. the plurality answer identified more discrete radio components and the SWIRE survey [13] from the 4. RGZ data products smaller but deeper field centeredsurvey on ELAIS [4] S1 taken and with the the CDFS. Australia Radio Telescope data Compact come Array from and the 3.6 ATLAS selects radio sources in thea FIRST catalog subset [3] of taken 174,821 with resolvedthe the 3.4 sources. Very Large Array, The which near-IR constitutes images matched to host galaxies come from Radio Galaxy Zoo volunteers and scientists in a discussion forum dubbed ‘Radio Talk’ PoS(EXTRA-RADSUR2015)008 Kyle W. Willett than normal ellipticals; this could be due either ] 6 5 . 0 > ) 3 W ´ nska et al, submitted). − 2 W [( 000 radio hosts identified from RGZ (black contours), overlaid on a subset of the , 33 ∼ Plot of Hybrid radio galaxies (HyMORs) are rare examples of radio galaxies which show differing Using RGZ data tagged in the Radio Talk interface, we have been able to identify 11 new Fanaroff-Riley (FR) morphologies on eitherbetween side the of host an populations active ofnature nucleus FRI/FRII vs. [15]. nurture galaxies hypotheses have for Since important radio-loudto the implications galaxies, test difference HyMORs on are different the unique physical effects test scenarios.50 of cases candidates that reported can However, in help such the galaxies literature. are extremely rare, withHyMORs fewer and than two additional candidates basedalso allowed on more FIRST stringent imaging. definitions The ofof how increased several to sample previous classify size candidates a has (Kapi HyMOR and revises the classifications 5.2 Radio galaxies with hybrid morphology all-sky sources from the WISE catalogloud (colorscale). galaxies Green dots [14], show while a the smallerX-ray comparison dashed and sample radio red of cross-matching. line radio- (Adapted indicates from the Figure location 10 of in [2].) an “AGN wedge” identified through Figure 3: Radio Galaxy Zoo colors consistent with elliptical galaxies,of QSOs, galaxies or with LIRGs. redder colors There is also a significant population to an association of radio emissionin with prep). star-formation, or to enhanced dust content (Willett et al., PoS(EXTRA-RADSUR2015)008 ). 4 2 Mpc, which Kyle W. Willett ∼ : Binned plot of the median Right 7 : examples of sharply-bent radio galaxies identified in RGZ. Images are FIRST and NVSS Left RGZ is assembling a large catalog of bent jets based on the automatic classifications. The KWW is grateful for travel support from the American Astronomical Society and financial Galaxies with radio jets can have their apparent position angle affected by a number of physical bending angle is determined bylarge selecting angular galaxies size, either and with thengalaxy multiple measuring and discrete the the edges components angle of or inwith the a the sharply-bent radio jets, plane hotspots. many of of Preliminary the whichangle results sky for are the reveal newly with sample a identified. as respect a large We to function are number offor the analyzing cluster-centric of galaxies distance; the host galaxies results closer average show bending to that the the bending increases center of the cluster, with a marked jump between 1–2 Mpc (Figure bending angle from 888 consensusthe double distance and/or to triple the sources nearestcorresponds identified optical roughly in to cluster. RGZ, the virial plotted A radius as sharp forbe a typical increase strongest. galaxy function in clusters, of where bending effects angle on jets occurs from near the ICM would aid from the organizers of the EXTRA-RADSUR2015 conference. Support was also provided by We attribute this to the combineddensity toward effects the of cluster higher center peculiar (Rudnick, velocities Willett, Garon and et an al., increase in in prep). the ICM 6. Acknowledgments images, zoomed out to show the full scale of the jets for each galaxy. Figure 4: interactions; one such effect arisesintracluster from medium the (ICM) peculiar due to motion ram of pressure.to the In result galaxy simulations, in higher with narrower relative tails, respect velocities which are to can shown Measuring depend a (on the dense average) jet on bending the distance angle to canand the yield merger center a history. of the powerful cluster. probe of the ICM pressure, dynamical state, Radio Galaxy Zoo 5.3 Jet bending angles PoS(EXTRA-RADSUR2015)008 . , PASA , 194:31, ApJS Kyle W. Willett , 140:1868–1881, AJ , 446:2985–3001, 2015. , 435:2835, November 2013. MNRAS , 451:1299–1305, August 2015. , 453:2326–2340, November 2015. , 132:2409–2423, December 2006. MNRAS AJ http://rgzauthors.galaxyzoo.org MNRAS , 389:1179–1189, September 2008. MNRAS , 363:507–516, November 2000. , 453:4020–4036, November 2015. 8 000 RGZ volunteers whose classifications make the , A&A MNRAS , 475:479–493, February 1997. MNRAS , 115:897–927, August 2003. ApJ PASP , 438:1149–1161, February 2014. MNRAS , 165:95–107, July 2006. ApJS 1 and their link with the quasar luminosity function. ∼ December 2010. Infrared Extragalactic Survey. radio-loud AGN. tions for the Fanaroff-Riley dichotomy. Explorer (WISE): Mission Description and Initial On-orbit Performance. June 2011. inspection of galaxies from the SDSS. classifications for 304,122 galaxies from the SDSS. Database. z S/Spitzer Wide-Area Infrared Extragalactic Field. geometry: application to SWIRE and ATLAS. Sources from the FIRST Survey. mosaics and component catalogues. 28:215–248, August 2011. morphologies derived from visual inspection. [9] D. D. Proctor. Morphological Annotations for Groups in the FIRST Database. [7] D. D. Proctor. Comparing Pattern Recognition Feature Sets for Sorting Triples in[8] theS. FIRST van Velzen, H. Falcke, and E. Körding. Nature and evolution of powerful radio galaxies at [6] R. P. Norris, J. Afonso, P. N. Appleton, et al. 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J. Lintott, S. P. Bamford, et al. Galaxy Zoo 2: detailed morphological References Radio Galaxy Zoo NSF AST 12-11295. We thank the moreproject than possible; 8 they are individually acknowledged at