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Interacting and Merging Galaxies F Site.Org/N E Rom Axy 7252 T NASA, Th Al fr Image T and h A NGC NGC Figu ttp eam om CS/WF cour ://h re Hib , 7252. 7469, of tak 1. u te bar 4 NGC C bb e sy Gal n image NGC Nor le d of Interacting and Merging Galaxies f site.org/n e rom axy 7252 t NASA, th al. s 4676 is s (c h ample (1994). i ttp: up ou s r an H. , rtes e e //h an stored wsc d F in d y ord Ar ub en eas of thi p bles ter/arc , f NASA, G. 299. t rom s is i s Illi te tu to . B Bottom dy org/news hiv ngw t - th he . and e/releas e T orth, le Hu op f 12 R t. ro bb an -ban ce M. M w es le n d os fr te /gal C d Heritage, midd t om Figure 1.4 Galaxy sample in this study. Top and middle row from left to right: Arp 256, r l am /arc images colored axy/in NGC 7469, NGC 4676 and Arp 299. Bottom row from left to right: IC 883, NGC 2623 and l p e le f h in, t NGC 7252. North is up, and east is to the left. Most colored images are restored from HST iv ro to e G. tak ACS/WFC images (courtesy of NASA, the Hubble Heritage, A. Evans and ESA, taken from w A. i t /r m ri e ractin f Hartig, e ages http://hubblesite.org/newscenter/archive/releases/galaxy/interacting/2008/16/image/a/, gh en Ev rom l e t: ase and courtesy of NASA, H. Ford, G. Illingworth, M. Clampin, G. Hartig, and the ACS Science an w ar i IC l s g/2008/16/image th s/2002/11/image Team, taken from http://hubblesite.org/newscenter/archive/releases/2002/11/image/d/). e e and f and t 883, CTIO r Image of NGC 7252 is restored from B- and R-band images taken with CTIO 4m telescope e to stored ES from Hibbard et al. (1994). the ri NGC gh A, 4m A t: tak CS f rom teles 2623 Ar Figure 1.4 Galaxy sample in this study. Top and middle row from left to right: Arp 256, e Some galaxies don’t fit the elliptical/spiral/irregular classification. Scie n p H 12 /d /a/, NGC 7469, NGC 4676 and Arp 299. Bottom row from left to right: IC 883, NGC 2623 and from cop 256, an n S /). c NGC 7252. North is up, and east is to the left. Most colored images are restored from HST T d e e ACS/WFC images (courtesy of NASA, the Hubble Heritage, A. Evans and ESA, taken from http://hubblesite.org/newscenter/archive/releases/galaxy/interacting/2008/16/image/a/, and courtesy of NASA, H. Ford, G. Illingworth, M. Clampin, G. Hartig, and the ACS Science Team, taken from http://hubblesite.org/newscenter/archive/releases/2002/11/image/d/). Image of NGC 7252 is restored from B- and R-band images taken with CTIO 4m telescope from Hibbard et al. (1994). Figure 1.4 Galaxy sample in this study. Top and middle row from left to right: Arp 256, NGCFigu7469,re 1.NGC4 Gal4676axy ansampled Arpin299.thisBottomstudy. roTopw franomd middleft toleriroghwt:fromIC 883,left NGCto righ2623t: Aranpd256, NGC 7469, NGC 4676 and Arp 299. Bottom row from left to right: IC 883, NGC 2623 and NGC 7252. North is up, and east is to the left. Most colored images are restored from HST 12 ACS/WFNGC C7252.imageNors (cthouisrtesupy, anofdNASA,east isthtoetHuhe bbleflet. Heritage,Most coloredA. Evimanagess andareESreA,storedtakefnromfromHST httpA://hCS/WFubbleCsite.org/nimages (cewscourtesenter/arcy of NASA,hive/releasthe Huesbb/galleaxy/inHeritage,teractinA. Evg/2008/16/imageans and ESA, tak/a/,en from andhcourttp://htesyuofbbNASA,lesite.org/nH. Fordewsc, G.enter/arcIllingwhivorth,e/releasM. Clesam/galpin,axy/inG. Hartig,teractinandg/2008/16/imagethe ACS Science/a/, Teamand, takcourentefromsy of hNASA,ttp://hH.ubFblesordi,teG..org/newsIllingworth,centeM.r/arcClamhivpein,/relG.easeHartig,s/2002/11/imageand the ACS/dScie/). nce ImageTeamof NGC, take7252n fromis rhestoredttp://hfubromblesBi-teand.org/newsR-banced nimagester/arctakhivene/rweliethaseCTIOs/2002/11/image4m telescop/de /). fromImageHibbarofdNGCet al.7252(1994).is restored from B- and R-band images taken with CTIO 4m telescope from Hibbard et al. (1994). Figure 1.4 Galaxy sample in this study. Top and middle row from left to right: Arp 256, NGC 7469, NGC 4676 and Arp 299. Bottom row from left to right: IC 883,12NGC 2623 and 12 NGC 7252. North is up, and east is to the left. Most colored images are restored from HST ACS/WFC images (courtesy of NASA, the Hubble Heritage, A. Evans and ESA, taken from http://hubblesite.org/newscenter/archive/releases/galaxy/interacting/2008/16/image/a/, and courtesy of NASA, H. Ford, G. Illingworth, M. Clampin, G. Hartig, and the ACS Science Team, taken from http://hubblesite.org/newscenter/archive/releases/2002/11/image/d/). Image of NGC 7252 is restored from B- and R-band images taken with CTIO 4m telescope from Hibbard et al. (1994). 12 How Galaxies Collide If galaxies move away from each other as the universe expands, how can they ever collide? Interacting Galaxy UGC 9618 The gravitational attraction of two massive galaxy halos can locally reverse the expansion and cause a collision. Most interacting pairs probably fell together “recently”. 1972ApJ...178..623T Tides between disk galaxies create filaments of stars. SPIN –0.5 0 0.5 1 1.5 2 2.5 3 Galactic Bridges and Tails The Mice: Two Colliding Spirals "The Mice": Colliding Galaxies NGC 4676: True-Color RGB Image Simulation of the Mice The Mice at Play Simulation of the Mice The Mice at Play Orbit Decay + 1. Spherical halos approach Orbit Decay + 1. Spherical halos approach 2. Tidal forces stretch halos Orbit Decay + 1. Spherical halos approach 2. Tidal forces stretch halos 3. Elongated halos are torqued Orbit Decay + 1. Spherical halos approach 2. Tidal forces stretch halos 3. Elongated halos are torqued 4. Halos spin up as orbit decays Why do Galaxies Merge? Tidal forces transform the organized orbital motion of galaxies into random motions of stars and dark matter. • This is a form of friction — it slows galaxies down. • Dark matter plays critical role — absorbs momentum. What Kind of Galaxy Results from a Merger? Random stellar orbits can naturally account for the oval shapes and slow rotation of elliptical galaxies. • Merger hypothesis: spiral galaxies merge to form elliptical galaxies. • Estimated merger rates can produce right number of elliptical galaxies. • Need additional star formation in mergers to form cores of elliptical galaxies. The Antennae Super Star Clusters in the Antennae Galaxies Rapid star formation is common in merging spiral galaxies! NGC 4038/4039 Simulation of the Antennae Antennae Simulation With Star Formation Antennae Simulation With Star Formation A Recent Merger Remnant: NGC 7252 THE [O III]NEBULA OF NGC 7252 3 Figure 1. Groundbased B and narrow-band [O III]andHα images of NGC 7252 obtained with the du Pont 2.5-m telescope. (a)High-contrastdisplayofB image, showing 6.!2 × 5.!7(120× 110 kpc2)fieldofview;theboxmarksthe3.!1 × 2.!85 (60 × 55 kpc2)areadisplayedinpanels(b)–(d).Noticethetwotidal tails connecting to loops around the main body. (b)PortionofB image displayed at twice enlarged scale relative to Panel (a). (c)and(d)Continuum-subtracted [O III] λ5007 and Hα emission-line images, reproduced at the same scale as Panel (b) and showing the distribution of ionized gas. Notice the [O III]nebulaSW of the nucleus in Panel (c). (e)and(f)Same[OIII]andHα images as in panels (c) and (d), but twice enlarged and reproduced at lower contrast. Details of the [O III]nebulaandoffiveHII regions in the W loop are better visible. Notice also the brightly Hα-emitting disk centered on the nucleus (black circular area). This ionized- and molecular-gas disk corresponds to the central “minispiral” observed on HST images; for details, see text. the area shown 2× enlarged in Figures 1b–1d.Thebottom ∼ 14 kpc west of the nucleus, best visible in the same two Hα two panels are enlarged 2× more, showing a region half the panels. size (and one quarter the area) of the box drawn in Figure 1a. The [O III]nebulosity(hereafter‘[OIII]nebula’)coversa Both the [O III] λ5007 and the Hα images had the galaxy con- projected area of about 10.1 × 6.6kpc2 (31.!!5 × 20.!!6) in the tinuum subtracted as described above. They are displayed at east–west and north–south directions, respectively, and ap- relatively high contrast in the middle two panels, and at lower pears brightest at a point lying about 4.0 kpc (12.!!4) west and contrast in the bottom two panels to show more details. No- 3.6 kpc (11.!!2) south of the nucleus. The apparent structure of tice the striking [O III]emissionnebulosityslightlybelowthe this [O III]nebulaisdiscussedinmoredetailin§3.1below. centers of panels (c) and (e), the bright central disk of Hα emission surrounding the nucleus of the galaxy (circular black areas in panels d and f), and the string of five H II regions 2.2. Spectroscopy NGC 7252: Data vs. Model M = 21.22 M = 20.68 B − B − U B = 0.17 U B = 0.16 − − B V = 0.66 B V = 0.60 − − V R = 0.74 V R = 0.52 − − NGC 7252: Star Formation History Starburst Galaxies Starburst Galaxy M82 Star formation rate: ~10 × Milky Way’s. Gas outflow driven by supernovae Galaxy Wars: M81 versus M82 Arp 299: Supernova Factory First encounter ~700 Myr ago Ultra-Luminous Infrared Galaxy 12 (L > 10 L⊙): Lopt ≈ 0.01 Lir Interacting Galaxy NGC 3690 Galaxies: Spectral7.1 Energy Groups: the Distributions homes of disk galaxies (SEDs) 291 Starlight “Hot” Dust Far IR Visible Mid.
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