Dark Matter. ASTR 333/433 Spring 2018 T R 4:00-5:15pm Sears 552
|
|
- Camron Horn
- 5 years ago
- Views:
Transcription
1 Dark Matter ASTR 333/433 Spring 2018 T R 4:00-5:15pm Sears 552 TODAY - Laws of Galactic Rotation - Flat rotation curves - Tully-Fisher - Universal Rotation curve - central Density Relation - Renzo s Rule - Radial acceleration relation
2 <latexit sha1_base64="ialy7qjdqlgolu5hksa9ic51xo8=">aaacbxicbvbps8mwhe39o+e/qkcvwshoy+hecn4gxjxosdtghsxn0i0stuvyq1lg7l78kl4ut4pxv4lfxmzrzzspao/3xkjecxlbntjor7wyura+svnykm7v7o7t2wehtr2nijkxxijw7ybojrhklnaqrj0orqjasfywvjn4ruemni/la2qj60akl3nikqej+fzzs3yppcx7aybkxu/y4zke7hxoa/qhb5ecijmfxibvnjrqjozv/3i9mkyrk0af0bptdrlojogctgubf71us4tqiemz0btggj8aqyfdwjkjau/vuryjtm6iwcqjago96e3e/7xocmgto+iysyfjonsotawgge82wt2ugawrguko4uahma6iihtmckvtvbpydjm4f5xrinn3warx8g0k6bidodkqoitur7eogvxe0qt6q5/oy3q2xq1362mwxbhyo0dodtb3h87zmak=</latexit> <latexit sha1_base64="ialy7qjdqlgolu5hksa9ic51xo8=">aaacbxicbvbps8mwhe39o+e/qkcvwshoy+hecn4gxjxosdtghsxn0i0stuvyq1lg7l78kl4ut4pxv4lfxmzrzzspao/3xkjecxlbntjor7wyura+svnykm7v7o7t2wehtr2nijkxxijw7ybojrhklnaqrj0orqjasfywvjn4ruemni/la2qj60akl3nikqej+fzzs3yppcx7aybkxu/y4zke7hxoa/qhb5ecijmfxibvnjrqjozv/3i9mkyrk0af0bptdrlojogctgubf71us4tqiemz0btggj8aqyfdwjkjau/vuryjtm6iwcqjago96e3e/7xocmgto+iysyfjonsotawgge82wt2ugawrguko4uahma6iihtmckvtvbpydjm4f5xrinn3warx8g0k6bidodkqoitur7eogvxe0qt6q5/oy3q2xq1362mwxbhyo0dodtb3h87zmak=</latexit> <latexit sha1_base64="ialy7qjdqlgolu5hksa9ic51xo8=">aaacbxicbvbps8mwhe39o+e/qkcvwshoy+hecn4gxjxosdtghsxn0i0stuvyq1lg7l78kl4ut4pxv4lfxmzrzzspao/3xkjecxlbntjor7wyura+svnykm7v7o7t2wehtr2nijkxxijw7ybojrhklnaqrj0orqjasfywvjn4ruemni/la2qj60akl3nikqej+fzzs3yppcx7aybkxu/y4zke7hxoa/qhb5ecijmfxibvnjrqjozv/3i9mkyrk0af0bptdrlojogctgubf71us4tqiemz0btggj8aqyfdwjkjau/vuryjtm6iwcqjago96e3e/7xocmgto+iysyfjonsotawgge82wt2ugawrguko4uahma6iihtmckvtvbpydjm4f5xrinn3warx8g0k6bidodkqoitur7eogvxe0qt6q5/oy3q2xq1362mwxbhyo0dodtb3h87zmak=</latexit> <latexit sha1_base64="fvkfok48asfc4kluekq/qcpzca0=">aaacgnicbvbns8mwae39npor6tflcajtw2hfcilcwivh+ve3wetj07qlsz9iuqwu/rqv/huve0+kf/+n2dblnh8ehu+9klznpywkari/2tlyyuraemwjurm1vbor7+0/istjmfg4yqnvekgqrmnissoz6aacomhjpomnbsz+55lwqzp4ueypcsiuxjsggeklufqv/uddclmfn8fd+j20oq37engevedjbf7dofcmthdcx9vrrsoyac4ssyq1uklt6ipbt3awkvhihotomuyqnqjxstejw6qdcziipeahksbdhvbyst4meq5olofencmhsig88lqyqriv5r2x+j/xy2tqdaoap5kkmz4+fgqmygsoh4i+5qrlliucmkfqhxd3eudyqjmrqro5x3srwgeny4zxd15rncsnkuaqhie6mmefaifb0aywwoanjmax+nzetxftq/ucrpe08s4bmih28wfc6z9h</latexit> <latexit sha1_base64="kplqs2jfrrw7+6xpvkrgfsmy4qi=">aaacsnicbvdns8mwhe3m1dm/qh69bifgxdeowxkqbl48zmg3wtplmqvbwppbkgqj9p/z4swbf4cxxyvpvovtpgg83ntjfr/nxzxjzzrvslrr3tzaruxud/f2dw6no+oujbjbqe0ihom+hyxllks2yortfiwodjxoe970lvd7z1rifowpahbtyydhifmzwuplrsgdakujcnjx5qa/3mmiy9atcnybsdp9aqxywdrj7csi4mrykiy5ctotthb9czuza9tmujkhwidwqwqgqns1xpxrrjkahopwloxammm1tpmhcadz1ukkjtgz4jfn511k6fxli+rhqp9qobm6lmobllpa08l8trnq5ej/3ibrfnoysjbofa3j4im/4uhfkc8wjzigrpgzjpgipidezij1p0rxx9wrw6ulrho7ub+pmw9xtvaz6kactsezuaawuaytca/awayevifpcgejvsip+aw/f9eslo6cgcwuyj++tlpj</latexit> <latexit sha1_base64="/h5zmxgp7dm9rh9xwligt3nlwco=">aaachxicbvdlsgmxfm3uv62vuzdugkwomzijgnuhfgrxwcgxhu4zmmmmdc08sdjcgfivbvwverrxivg3ztpx0cebwogce+49108yfdkyfo3syura+kz5s7k1vbo7z+4fpio45zg4ogyx7/hieeyj4kgqgekknkdqz6ttj25yv/1eukbx9cdhcemfabdrggiktesz126i5jch2ub52t+pfaeuvikzixgdt6q2loqjrtspz1atujubxcr2qaqgqmsz39x+jnoqrbizjetxthlzyxcxfdoikm4qsilwca1inqmn4imw+jciux6rhbn1jodcicahr5p5bmley8vlxjevqaox0shjjynwdfcqmihjmn8k9iknwlkxjghzqjeeeig4wljftkkr2/nff4lzvr+sw/fn1wajueezhifjuam2uabncadawaeyvib38aw+jwfj1fgwpqfrklh8oqqzmh7+acpfo7y=</latexit> <latexit sha1_base64="/h5zmxgp7dm9rh9xwligt3nlwco=">aaachxicbvdlsgmxfm3uv62vuzdugkwomzijgnuhfgrxwcgxhu4zmmmmdc08sdjcgfivbvwverrxivg3ztpx0cebwogce+49108yfdkyfo3syura+kz5s7k1vbo7z+4fpio45zg4ogyx7/hieeyj4kgqgekknkdqz6ttj25yv/1eukbx9cdhcemfabdrggiktesz126i5jch2ub52t+pfaeuvikzixgdt6q2loqjrtspz1atujubxcr2qaqgqmsz39x+jnoqrbizjetxthlzyxcxfdoikm4qsilwca1inqmn4imw+jciux6rhbn1jodcicahr5p5bmley8vlxjevqaox0shjjynwdfcqmihjmn8k9iknwlkxjghzqjeeeig4wljftkkr2/nff4lzvr+sw/fn1wajueezhifjuam2uabncadawaeyvib38aw+jwfj1fgwpqfrklh8oqqzmh7+acpfo7y=</latexit> <latexit sha1_base64="/h5zmxgp7dm9rh9xwligt3nlwco=">aaachxicbvdlsgmxfm3uv62vuzdugkwomzijgnuhfgrxwcgxhu4zmmmmdc08sdjcgfivbvwverrxivg3ztpx0cebwogce+49108yfdkyfo3syura+kz5s7k1vbo7z+4fpio45zg4ogyx7/hieeyj4kgqgekknkdqz6ttj25yv/1eukbx9cdhcemfabdrggiktesz126i5jch2ub52t+pfaeuvikzixgdt6q2loqjrtspz1atujubxcr2qaqgqmsz39x+jnoqrbizjetxthlzyxcxfdoikm4qsilwca1inqmn4imw+jciux6rhbn1jodcicahr5p5bmley8vlxjevqaox0shjjynwdfcqmihjmn8k9iknwlkxjghzqjeeeig4wljftkkr2/nff4lzvr+sw/fn1wajueezhifjuam2uabncadawaeyvib38aw+jwfj1fgwpqfrklh8oqqzmh7+acpfo7y=</latexit> <latexit sha1_base64="jmyzj3esgpoollcaanjp1vvkvnk=">aaab7xicbvddsgjbgp3w/sx+3oqymyejfej2i8guaigilrowavvqwwznz3vw9oez2ude1+im6krovxqf3qzr90btwmdhndn83/m8hdoplovxyg1sbm3v5hcle/shh0xz6lgl41qq6pcyx6ljyuk5i6ijmok0kwikq4/ttje6m/ntfyoki6nnnu5op8sdiawmykul1yy2ys0kukx35celputxxlnkva050dqxm1kcda3x/on5muldgincszrd20puf4kfyottaagxsppgmsidopmvo0xnwvjreav9ioxm6lioh1koq08nq6ygctwbif953vqftf6erumqaeqwg4kuixwjwxfkm0gj4mnnmbfmb4jieatmll5qqve3v4uue+eyelo1nq5k9vp2gzycwhmuwyzrqmmdnmabaim8wsd8gynxarwbh4tozsj+nmasjo8/eskmtw==</latexit> Empirical Laws of Galactic Rotation Flat rotation curves (Rubin-Bosma Law) Rotation curves tend asymptotically towards a constant rotation velocity that persists to indefinitely large radii: V (R!1)! V f Tully-Fisher relation (Luminous, Stellar Mass, and Baryonic TF relations) The baryonic mass of galaxies scales as the fourth power of the flat rotation velocity: M b = AVf 4 <latexit sha1_base64="n/zqwictykrswvnh8ie/bndvhwm=">aaab6xicbvdlsgnbeoynrxhfuy9ebopgkexkwhgqil68cbhma5j1mz3mjknmh870cihkj7wonhr/xl/wb5wke0liwubrvun3tz9iodg2f63c2vrg5lz+u7czu7d/udw8auo4vyw3wcxj1fap5ljeviecjw8nitpql7zld2+nfuufky3i6bfhcxdd2o9eibhfi7n3nk+uyq1pesftxsuw7li9a1kltkzkkkhufx+6vziliy+qsap1x7etdmduowcstwrdvpoesiht8/fs1qk5m1kpbleyl0iyuxdynnr6fpomgvic6gvvkv7ndvimqu5yremkpglzqueqcczk2pv0hoim5cgqypqwgxi2oioynncpmoroctfv0rgox5xth0qpvs1ukictoivzcoasanahdwgag2d4g0/4sqt1ar1bh/nozsr+hmmcro8/tk6mcq==</latexit> Rotation curve shape varies with luminosity (Persic-Salucci universal rotation curve ) The shape of rotation curves varies systematically with luminosity, declining mildly at high L and rising slowly at low L: V (R) =F (L, R d ) Central density relation (lower surface brightness galaxies exhibit larger mass discrepancies) The central dynamical surface densities of galaxies is related to their central surface brightnesses: dyn (R! 0) = f[ (R! 0)] Renzo s rule (Sancisi s Law) For any feature in the luminosity profile there is a corresponding feature in the rotation curve and vice versa. (Sancisi 2004). Radial acceleration relation (Milgrom s Law) The observed centripetal acceleration is related to that predicted by the observed distribution of baryons: g obs = F(g bar ) g bar = V bar 2 R
3 Rotation curves tend asymptotically towards a constant rotation velocity that persists to indefinitely large radii: V / const M R R 2 Optical data from Rubin, Thonnard, & Ford 1978, ApJ, 225, L107 Presumably this behavior cannot persist indefinitely, but there are no clear counter-examples.
4 Cases where rotation curves were thought to perhaps be declining have so far turned out to flatten. DDO 154 de Blok et al. (2008 [THINGS]): We do not find steep declines in velocity in the outer rotation curves of NGC 3521, NGC 7793, DDO 154, and NGC Where declines are observed, they are gentler, and (within the uncertainties in rotation velocity and inclination) consistent with flat rotation curves.
5 DDO 154 inclination
6 Mass models van Albada et al. (1985) V 2 tot = V 2 disk + V 2 halo
7 Tully-Fisher: Rotation curve amplitude correlates with observed mass: star dominated HSB gas dominated LSBs Flat rotation curves continue to occur in quite small systems (e.g., Leo P with Vf ~ 15 km/s)
8 Tully & Fisher (1977) Great for distance scale work. But why does it happen? Abs. Mag. line-width
9 Observables Luminosity (must calibrate with known D) Band pass (BVRIJHK) [slope varies with band] Mass - stars, gas, stars+gas Rotation Velocity line-widths; rotation curves W 20, W50; Vflat, V2.2, Vmax inclination corrections 1/ sin(i) turbulence/non-circular motions
10 Luminosity measures Band pass slope becomes steeper from bluer to redder bands (B I H) Worry about internal extinction, especially for blue bands and highly inclined galaxies Mass Can convert luminosity to stellar mass by estimating the stellar M/L via population modeling. IMF biggest systematic uncertainty
11 What we measure Luminosity Stellar Mass Gas: HI, H2 Rotation speed line-width rotation curve NGC 6946 Uncertainties Distance Stellar M*/L HI flux, X-factor velocity dispersion inclination asymmetric drift Vp Rotation curve data from Boomsma et al (2008) [HI] Daigle et al (2006) [Ha] Blais-Ouellette et al (2004) [ Mass model built from 2MASS K-band data (SSM) Vmax Vflat Vp V2.2
12 outer (flat) velocity maximum velocity peak velocity THINGS data (Walter et al 2008)
13 Velocity estimators: Vflat THINGS data (Walter et al 2008) W20 W50 Vp Different velocity measurements correlate but are not identical. TF relations fit using linewidths will differ from those fit using resolved rotation curves. W20 W50 Vmax
14 Tully-Fisher relation H-band Luminosity Bothun et al. (1985) Sakai et al. (2001) Luminosity and line-width are presumably proxies for stellar mass and rotation velocity. line-width
15 Stellar Mass Tully-Fisher relation Bothun et al. (1985) Sakai et al. (2001) nominal M*/L (Kroupa IMF) Stellar Mass M = M L L line-width
16 Stellar Mass Tully-Fisher relation Bothun et al. (1985) Sakai et al. (2001) double M*/L Stellar Mass...but stellar mass is completely dependent on choice of mass-tolight ratio (and degenerate with distance) line-width
17 Stellar Mass Tully-Fisher relation Bothun et al. (1985) Sakai et al. (2001) nominal M*/L Stellar Mass...but stellar mass is completely dependent on choice of mass-tolight ratio (and degenerate with distance) line-width
18 Stellar Mass Tully-Fisher relation Bothun et al. (1985) Sakai et al. (2001) half M*/L Stellar Mass...but stellar mass is completely dependent on choice of mass-tolight ratio (and degenerate with distance) line-width
19 Stark, McGaugh, & Swaters et al. (2009) If you want to use Vflat, you have to observe far enough out to measure it. log log R < 0.1 OK works well as a criterion. Scatter in TF increases as threshold weakened. marginal
20 Scatter in TF relation reduced with resolved rotation curves (Verheijen 2001) Stellar Mass TF Stellar Mass Stellar Mass line-width outer (flat) velocity
21 Stellar Mass TF Low mass galaxies tend to fall below extrapolation of linear fit to fast rotators (Matthews, van Driel, & Gallagher 1998; Freeman 1999) M = M L L Stellar Mass outer (flat) velocity
22 Gas Mass TF Gas mass by itself does NOT produce a good TF relation, at least for fast rotators. M g =1.4M HI Gas Mass outer (flat) velocity
23 Stellar Mass TF M = M L L Stellar Mass outer (flat) velocity
24 Baryonic TF Adding gas to stellar mass restores a single continuous relation for all rotators. M b = M + M g Baryonic Mass Baryonic mass is the important physical quantity. It doesn t matter whether the mass is in stars or in gas. outer (flat) velocity
25 Baryonic TF Twice Nominal M*/L Now instead of a translation, the slope pivots as we vary M*/L. Baryonic Mass Scatter increases as we diverge from the nominal M*/L. outer (flat) velocity
26 Baryonic TF Nominal M*/L Now instead of a translation, the slope pivots as we vary M*/L. Baryonic Mass Scatter increases as we diverge from the nominal M*/L. outer (flat) velocity
27 Baryonic TF Half Nominal M*/L Now instead of a translation, the slope pivots as we vary M*/L. Baryonic Mass Scatter increases as we diverge from the nominal M*/L. outer (flat) velocity
28 Baryonic TF Quarter Nominal M*/L Now instead of a translation, the slope pivots as we vary M*/L. Baryonic Mass Scatter increases as we diverge from the nominal M*/L. outer (flat) velocity
29 Baryonic TF Zero M*/L Now instead of a translation, the slope pivots as we vary M*/L. Baryonic Mass Scatter increases as we diverge from the nominal M*/L. outer (flat) velocity
30 Low mass galaxies considerably expand range of the TF relation. Gas dominated galaxies can provide absolute calibration of mass scale.
31 Gotta believe the data. Biggest challenge for low mass systems is the inclination e.g., Begum et al. (2008) estimate inclinations from both optical and HI morphology. Only half agree to within 12% in sin(i).
32 Trachternach et al. (2009) Example low line-width, gas dominated galaxies with M <M g optical HI
33 D500-3 Trachternach et al. (2009) D631-7 D512-2 D575-2
34 D646-7 D575-5 Trachternach et al. (2009) D575-1 D NO SIGNAL Note that you can measure a line-width even if there is no evidence of rotation.
35 Trachternach et al. (2009) rotation curves Systematic inclination errors bias data to left of the BTFR. (A galaxy can be face-on without looking perfectly circular.) line-widths
36 Stellar Mass Tully-Fisher relation X McGaugh et al. (2000) Begum et al. (2008) Trachternach et al. (2009) Gurovich et al. (2010) McGaugh (2005) Stark et al. (2009) Begum et al. (2008) Trachternach et al. (2009) gas dominated star dominated line-width outer (flat) velocity
37 HI Tully-Fisher relation X McGaugh et al. (2000) Begum et al. (2008) Trachternach et al. (2009) Gurovich et al. (2010) McGaugh (2005) Stark et al. (2009) Begum et al. (2008) Trachternach et al. (2009) gas dominated star dominated line-width outer (flat) velocity
38 Baryonic Tully-Fisher relation: slope & scatter depend on Velocity estimator slope: x = 3.5 slope: x = 4 X McGaugh et al. (2000) Begum et al. (2008) Trachternach et al. (2009) Gurovich et al. (2010) McGaugh (2005) Stark et al. (2009) Begum et al. (2008) Trachternach et al. (2009) gas dominated star dominated M,intrinsic 0.2 M,intrinsic < 0.15 finite intrinsic scatter negligible intrinsic scatter line-width outer (flat) velocity
39 Gas dominated galaxies can provide absolute calibration of mass scale. Gas Mass gas dominated star dominated Fraction of error budget due to systematics in M*/L Stellar Mass Baryonic Mass Systematic errors in M*/L no longer dominate the error budget for galaxies with Mg > M*.
40 Gas Rich Galaxy Baryonic Tully-Fisher relation (Stark et al 2009; Trachternach et al 2009; McGaugh 2011, 2012)
41 select M g >M try fits with many different combinations of IMF and populations synthesis models M b = A V f x slope x =3.94 ± 0.07 (random) ± 0.08 (systematic) Stark, McGaugh, & Swaters (2009, AJ, 138, 392) Fixing the slope to 4 gives A = 47 ± 6M km 4 s 4
42 <latexit sha1_base64="ljejr+f9sppxtmqjguxgru6z23q=">aaacanicbvdlssnafl2pr1pfuzdubqvgqqrssc6eggvdcbvmw2hqmewn7ddjg5mjuekwbvwvn4orxq/wf/wbj203bb0wcdjndpee48wcswvzv0zhzxvtfao4wdra3tndm/cpwjjkbke2ixgkoh6wlloq2ooptjuxodjwog17o+tcbz9rivkupqhxthsbhotmzwqrtbnmirngnrrbijn0haxkhtm+wcrtuf5jlutv0j3rza5ztirwznayqm5agwbtdm0fpx+rjkchihxl2a1aseqlwchgom1ktijpjmkid2g6yzchu031kr8j/ukfjuycdwdsjgnpo/ol5akwk/9p3ut59v7kwjhrncttrx7ckypqxgjqm0gj4mmnmbfmx4jieosolk6tpknxf4mua/u8clmx7mvlrn3wqrgo4bjooaox0ibbaiinbf7gdt7hy3g2xo1342nqlrizp4cwn8b3h1+xlgi=</latexit> <latexit sha1_base64="yg5pcubjlezfmhgevhlmsm5swnk=">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</latexit> a=0.8 V f 4 Slope 4 corresponds to an acceleration: hai =1.24 ± ms 2 GM b McGaugh (2011, 2012) selected gas rich galaxies histogram: data line: distribution expected from observational uncertainties. The data are consistent with zero intrinsic scatter. M < 0.15 dex
43 NGC 2403 UGC 128 Size/surface brightness variations from TF
44 No residuals from TF with size or surface density Same (M,V) but very different size and surface density which is strange, since V 2 = GM R
45 No residuals from TF with size or surface brightness (Zwaan et al 1995; Sprayberry et al 1995; McGaugh & de Blok 1998)
46 TF already edge-on projection of disk fundamental plane No residuals from TF with size or surface density for disks V 2 = GM R log(v ) log(r) = 1 2 expected slope (dotted line) Note: large range in size at a given mass or velocity
47 Baryonic TF Relation Fundamentally a relation between the baryonic mass of a galaxy and its rotation velocity M b = M* + Mg = 47 Vf 4 (McGaugh 2012) doesn t matter if it is stars or gas Intrinsic scatter negligibly small Can mostly be accounted for by the expected variation in stellar M*/L Physical basis of the relation remains unclear Relation has real physical units if slope has integer value - Slope appears to be 4 if Vflat is used.
Dark Matter. ASTR 333/433 Fall 2013 M T 4:00-5:15pm Sears 552. Prof. Stacy McGaugh Sears
Dark Matter ASTR 333/433 Fall 2013 M T 4:00-5:15pm Sears 552 Prof. Stacy McGaugh Sears 573 368-1808 stacy.mcgaugh@case.edu Empirical Laws of Galactic Rotation Homework 2 due Oct 15 midterm Oct 29 What
More informationLaws of Galactic Rotation. Stacy McGaugh Case Western Reserve University
Laws of Galactic Rotation Stacy McGaugh Case Western Reserve University UGC 2885 Galaxies NGC 2403 Huge dynamic range in 10 kpc Gravitationally self-bound entities composed of stars, gas, dust, [& dark
More informationThe Baryonic Tully-Fisher Relation
NRAO - TF35: Global Properties of HI in Galaxies Workshop - 1 April 2012 The Baryonic Tully-Fisher Relation Stacy McGaugh University of Maryland Tully & Fisher (1977) Abs. Mag. line-width 9/30/10 3/30/10
More informationBaryonic Masses from Rotation Curves. Stacy McGaugh University of Maryland
Unveiling the Mass - Extracting and Interpreting Galaxy Masses, Kingston, Ontario, 19 June 2009 Baryonic Masses from Rotation Curves Stacy McGaugh University of Maryland Rotation curves tend to become
More informationGalaxies in the Cosmic Web
Galaxies in the Cosmic Web Empirical Constraints on Halo Profiles from Rotation Curves Stacy McGaugh University of Maryland New Mexico State University, Las Cruces, 19 May 2006 1. Global Correlations:
More informationarxiv:astro-ph/ v1 14 Nov 2003
**TITLE** ASP Conference Series, Vol. **VOLUME***, **YEAR OF PUBLICATION** **NAMES OF EDITORS** The visible matter dark matter coupling arxiv:astro-ph/0311348v1 14 Nov 2003 Renzo Sancisi Osservatorio Astronomico,
More informationDark Matter in Dwarf Galaxies
Maryland Center for Fundamental Physics & Joint Space-Science Institute 26-28 May 2010 Advances in Theoretical and Observational Cosmology Dark Matter in Dwarf Galaxies Stacy McGaugh University of Maryland
More informationRotation curves of spiral galaxies
Rotation curves of spiral galaxies Rotation curves Mass discrepancy Circular velocity of spherical systems and disks Dark matter halos Inner and outer regions Tully-Fisher relation From datacubes to rotation
More informationDoes Low Surface Brightness Mean Low Density? W.J.G. de Blok. Kapteyn Astronomical Institute. P.O. Box AV Groningen. The Netherlands.
Does Low Surface Brightness Mean Low Density? W.J.G. de Blok Kapteyn Astronomical Institute P.O. Box 800 9700 AV Groningen The Netherlands and S.S. McGaugh Department of Terrestrial Magnetism Carnegie
More informationGMU, April 13, The Pros and Cons of Invisible Mass and Modified Gravity. Stacy McGaugh University of Maryland
GMU, April 13, 2007 The Pros and Cons of Invisible Mass and Modified Gravity Stacy McGaugh University of Maryland What gets us into trouble is not what we don t know. It s what we know for sure that just
More informationDark Matter. 4/24: Homework 4 due 4/26: Exam ASTR 333/433. Today. Modified Gravity Theories MOND
Dark Matter ASTR 333/433 Today Modified Gravity Theories MOND 4/24: Homework 4 due 4/26: Exam Not any theory will do - length scale based modifications can be immediately excluded as the discrepancy does
More informationarxiv:astro-ph/ v1 1 Mar 2000
The Baryonic Tully-Fisher Relation S.S. McGaugh 1, J.M. Schombert 2, G.D. Bothun 2, and W.J.G. de Blok 3,4 ABSTRACT arxiv:astro-ph/0003001v1 1 Mar 2000 We explore the Tully-Fisher relation over five decades
More informationScaling Relations of late-type galaxies
Scaling Relations of late-type galaxies - an observational perspective - Lecture I Lecture II Trends along the Hubble sequence Galaxy rotation curves Lecture III Tully-Fisher relations Marc Verheijen Kapteyn
More informationThe close link between baryons and dark matter in disc galaxies
The close link between baryons and dark matter in disc galaxies Federico Lelli Astronomy Department, Case Western Reserve University, Cleveland, Ohio, USA Main Collaborators: Stacy McGaugh (Case Western
More informationMOdified Newtonian Dynamics an introductory review. Riccardo Scarpa European Southern Observatory
MOdified Newtonian Dynamics an introductory review By Riccardo Scarpa European Southern Observatory Everything started in 1933 with the work by Zwicky on the Coma cluster of galaxies, but were galaxy rotation
More informationThe dark and visible matter content of low surface brightness disk galaxies Blok, W. J. G. de; McGaugh, S. S.
University of Groningen The dark and visible matter content of low surface brightness disk galaxies Blok, W. J. G. de; McGaugh, S. S. Published in: The Astrophysical Journal IMPORTANT NOTE: You are advised
More informationarxiv: v2 [astro-ph.co] 7 Dec 2011
Draft version December 9, 2011 Preprint typeset using L A TEX style emulateapj v. 5/2/11 THE BARYONIC TULLY-FISHER RELATION OF GAS RICH GALAXIES AS A TEST OF ΛCDM AND MOND Stacy S. McGaugh Department of
More informationarxiv:astro-ph/ v1 10 May 1998
Testing Modified Newtonian Dynamics with Low Surface Brightness Galaxies Rotation curve fits arxiv:astro-ph/9805120v1 10 May 1998 W.J.G. de Blok 1 and S.S. McGaugh 2 1 Kapteyn Astronomical Institute, P.O.
More informationPolar Ring Galaxies FINDING THE DARK HALO SHAPE BY CAROLINE VAN BORM
Polar Ring Galaxies FINDING THE DARK HALO SHAPE BY CAROLINE VAN BORM Papers (1) Polar ring galaxies and the Tully-Fisher relation: Implications for the dark halo shape Iodice, E.; Arnaboldi, M.; Bournaud,
More informationROE, Edinburgh, 20 April Observational Constraints on the Acceleration Discrepancy Problem. Stacy McGaugh University of Maryland
ROE, Edinburgh, 20 April 2006 Observational Constraints on the Acceleration Discrepancy Problem Stacy McGaugh University of Maryland What gets us into trouble is not what we don t know. It s what we know
More informationBlue Compact Dwarfs:
Blue Compact Dwarfs: is internal dynamics the key? I Zw 18 1 Federico Lelli 1 Marc Verheijen Filippo Fraternali1,2 Renzo Sancisi1,3 1 Kapteyn Institute, University of Groningen 2 Astronomy Dept., University
More informationarxiv:astro-ph/ v2 14 Feb 2002
Accepted to AJ LSB Galaxies and the Tully-Fisher Relation Aeree Chung arxiv:astro-ph/0202057v2 14 Feb 2002 Department of Astronomy, Columbia University, New York, NY 10027 archung@astro.columbia.edu J.
More informationGlobal Scaling Relations of Spiral Galaxies
Global Scaling Relations of Spiral Galaxies Aaron A. Dutton Max Planck Institute for Astronomy (MPIA), Heidelberg, Germany IAU 311, Galaxy Masses as constraints to Formation Models, Oxford, July 2014 Outline
More informationDark Matter. ASTR 333/433 Spring Today Stars & Gas. essentials about stuff we can see. First Homework on-line Due Feb. 4
Dark Matter ASTR 333/433 Spring 2016 Today Stars & Gas essentials about stuff we can see First Homework on-line Due Feb. 4 Galaxies are made of stars - D. Silva (1990) private communication Stars Majority
More informationUniversal Properties of Galactic Rotation Curves and a First Principles Derivation of the Tully-Fisher Relation
Universal Properties of Galactic Rotation Curves and a First Principles Derivation of the Tully-Fisher Relation James G. O Brien 1, Thomas L. Chiarelli 2, and Philip D. Mannheim 3 1 Department of Sciences,
More informationLecture Three: Observed Properties of Galaxies, contd.! Hubble Sequence. Environment! Globular Clusters in Milky Way. kpc
Hubble Sequence Lecture Three: Fundamental difference between Elliptical galaxies and galaxies with disks, and variations of disk type & importance of bulges Observed Properties of Galaxies, contd.! Monday
More informationarxiv: v1 [astro-ph.ga] 14 Dec 2015
Draft version December 16, 2015 Preprint typeset using L A TEX style emulateapj v. 01/23/15 THE SMALL SCATTER OF THE BARYONIC TULLY-FISHER RELATION Federico Lelli 1, Stacy S. McGaugh 1, James M. Schombert
More informationarxiv: v1 [astro-ph.co] 27 Jan 2009
Astronomy & Astrophysics manuscript no. 0516ms c ESO 2018 October 30, 2018 The rotation curves shapes of late-type dwarf galaxies R. A. Swaters 1,2,, R. Sancisi 3,4, T. S. van Albada 3, and J. M. van der
More informationarxiv: v1 [astro-ph.ga] 12 Dec 2018
Preprint 13 December 2018 Compiled using MNRAS LATEX style file v3.0 Is there a fundamental acceleration scale in galaxies? Zhe Chang, 1,2 Yong Zhou 1,2 1 Institute of High Energy Physics, Chinese Academy
More informationThe Radial Acceleration Relation of Galaxies
The Radial Acceleration Relation of Galaxies Federico Lelli ESO Fellow (Garching, Germany) In collaboration with Stacy McGaugh (Case Western Reserve University) James Schombert (University of Oregon) Marcel
More informationUniversity of Groningen. Understanding disk galaxies with the Tully-Fisher relation Ponomareva, Anastasia
University of Groningen Understanding disk galaxies with the Tully-Fisher relation Ponomareva, Anastasia IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish
More informationThe dynamics of face-on galaxies in MOND
Journal of Physics: Conference Series PAPER OPEN ACCESS The dynamics of face-on galaxies in MOND To cite this article: Garry W. Angus 2016 J. Phys.: Conf. Ser. 718 032001 View the article online for updates
More informationStellar Population Synthesis, a Discriminant Between Gravity Models
Stellar Population Synthesis, a Discriminant Between Gravity Models Akram Hasani Zonoozi Institute for Advanced Studies in Basic Sciences, IASBS Zanjan, Iran In collaboration with: H.Haghi & Y.Sobouti
More informationarxiv:astro-ph/ v4 29 Sep 2004
The Mass Discrepancy-Acceleration Relation: Disk Mass and the Dark Matter Distribution Stacy S. McGaugh Department of Astronomy, University of Maryland arxiv:astro-ph/0403610v4 29 Sep 2004 College Park,
More informationOn the Keplerian Rotation Curves of Galaxies
PASJ: Publ. Astron. Soc. Japan 49,?? (1997) On the Keplerian Rotation Curves of Galaxies Mareki Honma and Yoshiaki Sofue Institute of Astronomy, Faculty of Science, The University of Tokyo, Mitaka, Tokyo,
More informationGalaxies Astro 530 Prof. Jeff Kenney
Galaxies Astro 530 Prof. Jeff Kenney CLASS 7 February 5, 2018 Tully-Fisher Relation (finish) & Spiral Structure (start) 1 Tully-Fisher relation M B,i Tradi7onal Tully- Fisher rela7on: Good correla7on between
More informationLecture Three: Observed Properties of Galaxies, contd. Longair, chapter 3 + literature. Monday 18th Feb
Lecture Three: Observed Properties of Galaxies, contd. Longair, chapter 3 + literature Monday 18th Feb 1 The Hertzsprung-Russell Diagram magnitude colour LOW MASS STARS LIVE A VERY VERY LONG TIME! 2 The
More informationarxiv: v2 [astro-ph.ga] 3 Jul 2018
Astronomy & Astrophysics manuscript no. FitRAR c ESO 218 July 4, 218 Fitting the radial acceleration relation to individual SPARC galaxies Pengfei Li 1, Federico Lelli 2,, Stacy S. McGaugh 1, and James
More informationTHE MASSES OF DISKS. Piet van der Kruit Kapteyn Astronomical Institute University of Groningen the Netherlands
THE MASSES OF DISKS Kapteyn Astronomical Institute University of Groningen the Netherlands Unveiling the mass, Kingston, Ontario, June 2009 Outline Why do we want to know the disk mass? Maximum disk hypothesis
More informationSe-Heon Oh. Se-Heon Oh
High-resolution mass models of rotation curves & LITTLE THINGS 1,2 1. International Centre for Radio Astronomy Research (ICRAR) The University of Western Australia 2. ARC Centre for All-sky Astrophysics
More informationUsing globular clusters to test gravity in the weak acceleration regime
Using globular clusters to test gravity in the weak acceleration regime Riccardo Scarpa 1, Gianni Marconi 2, Roberto Gilmozzi 2, and Giovanni Carraro 3 1 Instituto de Astrofísica de Canarias, Spain 2 European
More informationLow Surface Brightness Galaxies Erwin de Blok. Encyclopedia of Astronomy & Astrophysics P. Murdin
eaa.iop.org DOI: 10.1888/0333750888/2620 Low Surface Brightness Galaxies Erwin de Blok From Encyclopedia of Astronomy & Astrophysics P. Murdin IOP Publishing Ltd 2006 ISBN: 0333750888 Institute of Physics
More informationDark Matter in Disk Galaxies
Chapter 14 Dark Matter in Disk Galaxies Rotation curves of disk galaxies rise steeply in their inner regions and then remain roughly flat out to the last point measured. To explain these observations within
More informationHI studies of Low Surface Brightness Galaxies with the Nancay Radio Telescope
HI studies of Low Surface Brightness Galaxies with the Nancay Radio Telescope Honey M Indian Institute of Astrophysics, Bangalore Collaborators Dr. Jean-Michel Martin Observatoire Paris-Site de Meudon,
More informationThesis defence Friday 11:00
Thesis defence Friday 11:00 Promotors: Marc Verheijen Filippo Fraternali In collaboration with: Renzo Sancisi Outline: Introduction on (starbursting) dwarfs (Chap. 1) I. Large-scale HI morphology (Chaps.
More information11. Virial Theorem Distances of Spiral and Elliptical Galaxies
Virial Theorem 11. Virial Theorem Distances of Spiral and Elliptical Galaxies v 2 rot = s G M(R 0) R 0 2 = e G M(R eff ) R eff (s1) spiral galaxies (e1) elliptical galaxies v rot rotational velocity of
More informationThe Empirical Laws of Galactic Rotation
The Empirical Laws of Galactic Rotation Federico Lelli (ESO Fellow Garching, Germany) Main Collaborators: Stacy McGaugh (CWRU), James Schombert (Univ. of Oregon) Marcel Pawlowski (UCI), Filippo Fraternali
More informationEverything in baryons?
Everything in baryons? Benoit Famaey (ULB) Rencontres de Blois 2007 General Relativity -> Dark Matter R αβ - 1/2 R g αβ + Λg αβ = (8πG/c 4 ) T αβ very precisely tested on solar system scales (but Pioneer)
More informationarxiv: v1 [astro-ph.co] 11 Jul 2012
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 9 March 2013 (MN LATEX style file v2.2) The Link between the Baryonic Mass Distribution and the Rotation Curve Shape arxiv:1207.2729v1 [astro-ph.co]
More informationSurface Brightness of Spiral Galaxies
Surface Brightness of Spiral Galaxies M104: SA N4535: SAB LMC: dwarf irregular,barred Normal 1/4-law+exp fits An example of surface brightness profile. The top curve is the sum of exp disk+1/4-bulge. The
More informationarxiv: v1 [astro-ph] 13 May 2008
Draft version May 13, 28 Preprint typeset using L A TEX style emulateapj v. 8/13/6 MOND AND THE UNIVERSAL ROTATION CURVE: SIMILAR PHENOMENOLOGIES Gianfranco Gentile 1,2 Draft version May 13, 28 arxiv:85.1731v1
More informationThere are three main ways to derive q 0 :
Measuring q 0 Measuring the deceleration parameter, q 0, is much more difficult than measuring H 0. In order to measure the Hubble Constant, one needs to derive distances to objects at 100 Mpc; this corresponds
More informationMorphological Type Dependence in the Tully-Fisher Relationship
1 Morphological Type Dependence in the Tully-Fisher Relationship Abstract David G. Russell Owego Free Academy, Owego, NY 13827 USA russeld1@oagw.stier.org The Tully-Fisher relationship is subject to morphological
More informationThe modest! -values, as implied by the blue colors and
THE ASTRONOMICAL JOURNAL, 122:2396È2427, 2001 November ( 2001. The American Astronomical Society. All rights reserved. Printed in U.S.A. V HIGH-RESOLUTION ROTATION CURVES OF LOW SURFACE BRIGHTNESS GALAXIES.
More informationarxiv: v1 [astro-ph.ga] 14 Sep 2017
arxiv:1709.04918v1 [astro-ph.ga] 14 Sep 2017 Galaxy rotations from quantised inertia and visible matter only. M.E. McCulloch September 18, 2017 Abstract It is shown here that a model for inertial mass,
More information12.1 Elliptical Galaxies
12.1 Elliptical Galaxies Elliptical Galaxies Old view: ellipticals are boring, simple systems Ellipticals contain no gas & dust Ellipticals are composed of old stars Ellipticals formed in a monolithic
More informationASTR 610 Theory of Galaxy Formation Lecture 18: Disk Galaxies
ASTR 610 Theory of Galaxy Formation Lecture 18: Disk Galaxies Frank van den Bosch Yale University, spring 2017 The Structure & Formation of Disk Galaxies In this lecture we discuss the structure and formation
More informationSet 5: Expansion of the Universe
Set 5: Expansion of the Universe Cosmology Study of the origin, contents and evolution of the universe as a whole Expansion rate and history Space-time geometry Energy density composition Origin of structure
More informationWhittle : EXTRAGALACTIC ASTRONOMY 5. SPIRAL GALAXIES
Whittle : EXTRAGALACTIC ASTRONOMY 1 : Preliminaries 6 : Dynamics I 11 : Star Formation 16 : Cosmology : Morphology 7 : Ellipticals 1 : Interactions 17 : Structure Growth 3 : Surveys 8 : Dynamics II 13
More informationThe maximum rotation of a galactic disc
Astron. Astrophys. 328, 517 525 (1997) ASTRONOMY AND ASTROPHYSICS The maximum rotation of a galactic disc Roelof Bottema Kapteyn Astronomical Institute, P.O. Box 800, 9700 AV Groningen, The Netherlands
More informationDYNAMICAL STABILITY AND ENVIRONMENTAL INFLUENCES IN LOW SURFACE BRIGHTNESS DISK GALAXIES
THE ASTROPHYSICAL JOURNAL, 477 : L79 L83, 1997 March 10 1997. The American Astronomical Society. All rights reserved. Printed in U.S.A. DYNAMICAL STABILITY AND ENVIRONMENTAL INFLUENCES IN LOW SURFACE BRIGHTNESS
More informationGalaxy rotations from quantised inertia and visible matter only
Astrophys Space Sci (2017 362:149 DOI 10.1007/s10509-017-3128-6 ORIGINAL ARTICLE Galaxy rotations from quantised inertia and visible matter only M.E. McCulloch 1 Received: 3 March 2017 / Accepted: 26 June
More informationW hat gets us into trouble is not what we donït know. ItÏs what we know for sure that just ainït so. Yogi Berra
THE ASTROPHYSICAL JOURNAL, 499:41È65, 1998 May 2 ( 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. TESTING THE DARK MATTER HYPOTHESIS WITH LOW SURFACE BRIGHTNESS GALAXIES
More informationAy 127 Systematics of Galaxy Properties and Scaling Relations
Ay 127 Systematics of Galaxy Properties and Scaling Relations Morphological Classification and Galaxy Types The first step in any empirical science: look for patterns and trends, then try to understand
More informationarxiv:astro-ph/ v1 20 Nov 1996
PASJ: Publ. Astron. Soc. Japan 48,?? (2018) Mass of the Galaxy Inferred from Outer Rotation Curve Mareki Honma and Yoshiaki Sofue Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo,
More informationSpatial distribution of stars in the Milky Way
Spatial distribution of stars in the Milky Way What kinds of stars are present in the Solar neighborhood, and in what numbers? How are they distributed spatially? How do we know? How can we measure this?
More informationRelationship Between Newtonian and MONDian Acceleration
Advances in Applied Physics, Vol. 4, 2016, no. 1, 31-37 HIKARI Ltd, www.m-hikari.com http://dx.doi.org/10.12988/aap.2016.6810 Relationship Between Newtonian and MONDian Acceleration A. S. Sarabi Department
More informationarxiv:astro-ph/ v1 22 Jul 2002
1 arxiv:astro-ph/0207469v1 22 Jul 2002 Abstract. Rotation curves for four spiral galaxies with recently determined Cepheid-based distances are reconsidered in terms of modified Newtonian dynamics (MOND).
More informationAS1001:Extra-Galactic Astronomy
AS1001:Extra-Galactic Astronomy Lecture 5: Dark Matter Simon Driver Theatre B spd3@st-andrews.ac.uk http://www-star.st-and.ac.uk/~spd3 Stars and Gas in Galaxies Stars form from gas in galaxy In the high-density
More informationARE DWARF GALAXIES DOMINATED BY DARK MATTER?
C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. doi:10.1088/0004-637x/729/2/118 ARE DWARF GALAXIES DOMINATED BY DARK MATTER? R. A. Swaters 1,4, R. Sancisi 2,3, T.
More informationarxiv:astro-ph/ v1 16 Apr 2003
Mon. Not. R. Astron. Soc. 000, 1 14 (2002) Printed 17 April 2003 (MN LATEX style file v1.4) Chemical and spectrophotometric evolution of Low Surface Brightness galaxies arxiv:astro-ph/0304313 v1 16 Apr
More informationReview of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
More informationProbing Gravity in the Low Acceleration Regime with Globular Clusters
Probing Gravity in the Low Acceleration Regime with Globular Clusters By Riccardo Scarpa Instituto de astrofisica de Canarias Gran Telescopio Canarias The idea for this study sparked from the desire of
More informationSelf-Interacting Dark Matter
Self-Interacting Dark Matter James Bullock UC Irvine Garrison-Kimmel, Oñorbe et al. Act I Motivations Missing Satellites Problem (1999) Theory: N>>1000 Klypin et al. 1999; Moore et al. 1999; Kauffmann
More informationStellar Population Mass Estimates. Roelof de Jong (STScI AIP) Eric Bell (MPIA Univ. of Michigan)
Stellar Population Mass Estimates Roelof de Jong (STScI AIP) Eric Bell (MPIA Univ. of Michigan) Overview Stellar Mass-to-Light (M/L) ratios from SEDs Comparing different SED fitting techniques Comparing
More informationThe mass distribution in spiral galaxies
The mass distribution in spiral galaxies Irina Yegorova SISSA, Trieste, Italy In collaboration with Paolo Salucci, Alessandro Pizzella, Niv Drory Outline: The disk mass of spiral galaxies Radial Tully-Fisher
More informationarxiv: v2 [astro-ph.ga] 23 Jan 2017
Draft version January 25, 2017 Preprint typeset using L A TEX style emulateapj v. 01/23/15 ONE LAW TO RULE THEM ALL: THE RADIAL ACCELERATION RELATION OF GALAXIES Federico Lelli 1,2,, Stacy S. McGaugh 1,
More informationGalaxy Inclination and Surface Brightness
From the SelectedWorks of Jordan Rozum 2013 Galaxy Inclination and Surface Brightness Jordan C Rozum, Utah State University Shane L Larson, Utah State University Available at: https://works.bepress.com/jordan_rozum/4/
More informationASTR 200 : Lecture 22 Structure of our Galaxy
ASTR 200 : Lecture 22 Structure of our Galaxy 1 The 'Milky Way' is known to all cultures on Earth (perhaps, unfortunately, except for recent city-bound dwellers) 2 Fish Eye Lens of visible hemisphere (but
More informationTHE ASTRONOMICAL JOURNAL, 122:2381È2395, 2001 November ( The American Astronomical Society. All rights reserved. Printed in U.S.A.
THE ASTRONOMICAL JOURNAL, 122:2381È2395, 21 November ( 21. The American Astronomical Society. All rights reserved. Printed in U.S.A. V HIGH-RESOLUTION ROTATION CURVES OF LOW SURFACE BRIGHTNESS GALAXIES.
More informationMODIFIED NEWTONIAN DYNAMICS AS AN ALTERNATIVE TO DARK MATTER
Annu. Rev. Astron. Astrophys. 2002. 40:263 317 doi: 10.1146/annurev.astro.40.060401.093923 Copyright c 2002 by Annual Reviews. All rights reserved MODIFIED NEWTONIAN DYNAMICS AS AN ALTERNATIVE TO DARK
More informationThe Local Group Timing Argument
The Local Group Timing Argument Real galaxies Milky Way (MW) Andromeda (M31) Indranil Banik (ib45@st-andrews.ac.uk) Supervisor: Hongsheng Zhao University of Saint Andrews MNRAS, 467 (2), 2180 2198 Basic
More informationMODIFIED NEWTONIAN DYNAMICS AS AN ALTERNATIVE TO DARK MATTER
MODIFIED NEWTONIAN DYNAMICS AS AN ALTERNATIVE TO DARK MATTER Robert H. Sanders 1 & Stacy S. McGaugh 2 1 Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands 2 Department
More informationCLASSIFICATION OF SPIRAL GALAXIES ON THE BASIS OF ABSOLUTE MAGNITUDE
CLASSIFICATION OF SPIRAL GALAXIES ON THE BASIS OF ABSOLUTE MAGNITUDE N. Thakre Assistant Professor Mahakal Group of Institutes, Ujjain M. Thakre Research Scholar Mahakal Group of Institutes, Ujjain ABSTRACT
More informationImpact of Molecular Gas on the Mass Models of Nearby Galaxies
Netherlands Institute for Radio Astronomy Impact of Molecular Gas on the Mass Models of Nearby Galaxies Frank, de Blok, Walter, Leroy and Carignan, 2015 submitted* PHISCC 2015 ASTRON is part of the Netherlands
More informationAre Low Surface Brightness Discs Young?
Are Low Surface Brightness Discs Young? Paolo Padoan Theoretical Astrophysics Center, Juliane Maries Vej 30, DK-2100 Copenhagen, DK Raul Jimenez arxiv:astro-ph/9609091v1 12 Sep 1996 Royal Observatory,
More informationModified Newtonian Dynamics (MOND) and the Bullet Cluster (1E )
Modified Newtonian Dynamics (MOND) and the Bullet Cluster (1E 0657-558) Alan G. Aversa ABSTRACT Modified Newtonian Dynamics (MOND) is a theory that modifies Newton s force law to explain observations that
More informationRadial Distributions of Surface Mass Density and Mass-to-Luminosity Ratio in Spiral Galaxies
Publ. Astron. Soc. Japan (204) 00(0), doi:.93/pasj/xxx000 Radial Distributions of Surface Mass Density and Mass-to-Luminosity Ratio in Spiral Galaxies Yoshiaki SOFUE Institute of Astronomy, The University
More informationDark Matter: Observational Constraints
Dark Matter: Observational Constraints Does Dark Matter Exist? Leo Blitz UC Berkeley Stanford July 30, 2007 Questions I ll be addressing Does dark matter exist? Where do we know it does not exist? How
More informationEstimates of the Enclosed Mass and its Distribution. for several Spiral Galaxies. Abstract
Estimates of the Enclosed Mass and its Distribution for several Spiral Galaxies Geoffrey M. Williams email: gmwill@charter.net Abstract Recently, high quality rotation curves for several spiral galaxies
More informationSurface Photometry Quantitative description of galaxy morphology. Hubble Sequence Qualitative description of galaxy morphology
Hubble Sequence Qualitative description of galaxy morphology Surface Photometry Quantitative description of galaxy morphology Galaxy structure contains clues about galaxy formation and evolution Point
More informationUpcoming class schedule
Upcoming class schedule Thursday March 15 2pm AGN evolution (Amy Barger) th Monday March 19 Project Presentation (Brad) nd Thursday March 22 postponed to make up after spring break.. Spring break March
More informationUniversity of Groningen. Understanding disk galaxies with the Tully-Fisher relation Ponomareva, Anastasia
University of Groningen Understanding disk galaxies with the Tully-Fisher relation Ponomareva, Anastasia IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish
More informationEstimates of the Enclosed Mass and its Distribution. for several Spiral Galaxies. Abstract
Estimates of the Enclosed Mass and its Distribution for several Spiral Galaxies Geoffrey M. Williams email: gmwill@charter.net Abstract Recently, high quality rotation curves for several spiral galaxies
More informationProbing Gravity in the Low Acceleration Regime with Globular Clusters
Probing Gravity in the Low Acceleration Regime with Globular Clusters By Riccardo Scarpa, Gianni Marconi & Roberto Gilmozzi European Southern Observatory The idea of this study sparked from the following
More informationA unified multi-wavelength model of galaxy formation. Carlton Baugh Institute for Computational Cosmology
A unified multi-wavelength model of galaxy formation Carlton Baugh Institute for Computational Cosmology M81 Angel Lopez Sanchez A unified multi-wavelength model of galaxy formation Lacey et al. 2015 arxiv:1509.08473
More informationPhys/Astro 689: Lecture 8. Angular Momentum & the Cusp/Core Problem
Phys/Astro 689: Lecture 8 Angular Momentum & the Cusp/Core Problem Summary to Date We first learned how to construct the Power Spectrum with CDM+baryons. Found CDM agrees with the observed Power Spectrum
More informationPractice Problem!! Assuming a uniform protogalactic (H and He only) cloud with a virial temperature of 10 6 K and a density of 0.
Practice Problem Assuming a uniform protogalactic (H and He only) cloud with a virial temperature of 10 6 K and a density of 0.05 cm -3 (a) estimate the minimum mass that could collapse, (b) what is the
More informationarxiv:astro-ph/ v1 11 Dec 1996
To appear in the Astrophysical Journal Letters Dynamical Stability and Environmental Influences in Low Surface Brightness Disk Galaxies arxiv:astro-ph/9612115v1 11 Dec 1996 J. Christopher Mihos, 1,2 Stacy
More informationPhysics of Galaxies 2016 Exercises with solutions batch I
Physics of Galaxies 2016 Exercises with solutions batch I 1. Distance and brightness at low redshift You discover an interesting galaxy in the local Universe and measure its redshift to be z 0.053 and
More information