Ando_JournalClub_160708

Size: px
Start display at page:

Download "Ando_JournalClub_160708"

Transcription

1 Independent discoveries of a tidally disrupting dwarf galaxy around NGC 253! A Tidally Disrupting Dwarf Galaxy in the Halo of NGC 253 Toloba, E. et al. 2016, ApJL, 816, L5 (hereafter T16, accepted ) ( Satellite accretion in action: a tidally disrupting dwarf spheroidal around the nearby spiral galaxy NGC 253 Romanowsky, A. J. et al. 2016, MNRAS, 457, L103 (hereafter R16, accepted ) ( Journal Club Ryo Ando (IoA, UTokyo)

2 (R16) (T16)

3 Introduction ΛCDM model Halo substructure ( stellar streams) Local Group ( ) e.g. M81, NGC3109, M101; ( ) Milky Way random infall? low-surface brightness imaging + resolved stellar maps (10-50 cm) + CCD

4 Discovery of Scl-MM-Dw2 (T16) PISCeS Survey (Panoramic Imaging Survey of Centaurus and Sclptor) Magellan Clay 6.5 m Telescope (Las Campanas) Megacam (FoV: 24 x 24 / 0.16 pixel) Observation: PSF: g & r band, 6 x 300 s mag DSS Image Scl-MM-Dw2 150 kpc NGC (w/ diffuse light) 2. RGB stellar map NGC 253 Scl-MM-Dw2 NGC 253 NGC 253 PISCeS survey (T16) half-light radius background field ( ) Magellan Telescope (

5 Color-magnitude diagram (T16) All stars within the half-light radius - Background stars = [Fe/H] = -2.3 dex 12 Gyr isochrones [Fe/H] = -1.1 dex Residual AGB stars RGB stars (T16) Half-light radius - = Scl-MM-Dw2 3.1 ± 0.2 Mpc (NGC 253 consistent) TRGB (Tip of Red Giant Branch) ( ) CMD ( ) isochrone ( ) Age = 12 Gyr, [Fe/H] = -2.3 dex / -1.1 dex AGB RGB

6 Stellar distribution (T16) (black) (red) Scl-MM-Dw2 RGB (T16) AGB /RGB (2-3 Gyr) (-2.3 < [Fe/H] < (~ 12 NGC 253 halo Total stellar mass ~ (1.0 ± 0.4) x 10 7 M

7 Properties of the dwarf (T16) Green Bank Telescope HIPASS (HI Parkes All Sky Survey) data ~ 3.7 σ emission peak? GBT (Green Bank Telescope, 100 m) DDT non-detection HIPASS detection HI mass ~ 1.2 x 10 5 M, gas fraction M HI /L V < 0.02 M /L gas poor ( Structural parameters (T16) RGB Free parameters: (RA, DEC), PA, ε, r h, Σ b Large, elongated, very diffuse ε ~ 0.66 Sagittarius dwarf

8 Scaling Relations (T16) Total luminosity M V = ± 0.5 r h, r h (1-ε) aperture photometry ( ) Luminosity scaling relations Scl-MM-Dw2 ( ) Size Ellipticity ( Sgr dwarf ) Surface brightness (ultra-diffuse galaxies ) Large, elongated, very diffuse

9 Discovery of NGC 253-dw2 (R16) 18 cm 12 inch (30 cm) CHART32 real (80 cm & Subaru 8 m) CHART32 (Chilean Advanced Robotic Telescope) 80 Cerro Tololo FoV: 22 x 22 / pixel Observation: 2013 total exposure: s ( (R16) CHART32 image (80 cm) 8 kpc diffuse (dsph) ( ) Galactic cirrus Amateur Image (30 cm)

10 Discovery of NGC 253-dw2 (R16) (80 cm & Subaru 8 m) Subaru Suprime-Cam g band (5 x 114 s) & R c band (5 x 120 s) Observation: 2014 Subaru/Suprime-Cam image (5 x 18 ) Subaru Telescope ( Rc band star map (R16)

11 Color-magnitude diagram (R16) Rc band star map - = 13 Gyr isochrones (R16) Half-light radius - = r 0 ~ 25, (g-r) 0 ~ Mpc (NGC 253 consistent) RGB NGC 253 halo ( ) dsph - dirr RGB (1 Gyr ) ( 600 Myr ) isochrone [Z/H] ~ -2.0 ± 0.5

12 Properties of the dwarf (R16) Structural parameters free parameters: (RA, DEC), PA, ε, a h, N * ( (PDF) ) a h = 2.0 ± 0.4 kpc Probability density function (R16) Star counts Model fit (ε ~ ) L V = (1.6 ± 0.3) x 10 6 L (M V = ± 0.4 ) Disrupting dwarfs NGC 253-dw2 ( dsph 2 ) Disrupting dwarfs Half-light radius Absolute magnitude

13 Toloba et al Analyses and Results Romanowsky et al (T16) (R16)

14 Discussion & Conclusion Gas-poor dwarf spheroidal satellite galaxy Low gas fraction (M HI /L V < 0.02 M /L ) Large, elongated, diffuse Tidal disruption ( ) (dsph) ε > 0.6 dsph (e.g. Sgr, Her, UMa I & II) (T16) NGC 253 NGC 253 elongation Scl-MM-Dw2 / NGC 253-dw2 NGC 253 tidal tail (T16) 90%? (R16) > 2 x 10 7 L

15 Discussion & Conclusion NGC 253 (R16) (disrupting dsph) (dissolution dynamics) ( ) infall shear field (R16) (R16) NGC 253 recent unidentified interaction central starburst, kinematic twisting, stellar halo shelf Pre-infall virial mass (1-4 x M, ΛCDM model) ~ M * of NGC 253 (1.7 x M ) NGC 253 NGC 253-dw2? deep/wide-field stealth attacks

SFN

SFN THE STAR FORMATION NEWSLETTER No.291-14 March 2017 2017/04/28 16-20 16. X-Shooter spectroscopy of young stellar objects in Lupus. Atmospheric parameters, membership and activity diagnostics 17. The evolution

More information

MW鹿児島

MW鹿児島 NGC1068 Dark Matter Halo baryon gas stars SMBH SMBH 1 SMBHs? (AGN) AGN Seyfertization Taniguchi 1987, ApJ, 317, L57 AGN The dead quasar problem (Rees 1990, Science, 247, 817) T AGN ~ 10 8 yrs AGN AGN

More information

SuperMassive Black Holes

SuperMassive Black Holes Hello! Galaxy Morphology, Galaxies Near and Far SuperMassive Black Holes and all that Ajit Kembhavi IUCAA, Pune Galaxy Morphology, Galaxies Near and Far SuperMassive Black Holes and all that Ajit Kembhavi

More information

爆発的星形成? AGN関係を 生み出す物理機構の観測的示唆

爆発的星形成? AGN関係を 生み出す物理機構の観測的示唆 Umemura, Fukue & Mineshige 1997, 1998 Ohsuga et al. 1998 R ring ~100pc dv r = v 2 ϕ dt r 1 dp ρ dr dφ 1 r d(rv ϕ ) dt = 3χE 2c typical timescale dr + χ c F r 3 2 Myr r R ring V ring 3χE 2c v ϕ Umemura,

More information

Contents 1. Ia? 2. Ia 3. WISH Ia cosmology 4. WISH Ia + rate 5.

Contents 1. Ia? 2. Ia 3. WISH Ia cosmology 4. WISH Ia + rate 5. Type Ia Supernova Survey w/ WISH Contents 1. Ia? 2. Ia 3. WISH Ia cosmology 4. WISH Ia + rate 5. Contents 1. Ia? 2. Ia 3. WISH Ia cosmology 4. WISH Ia + rate 5. Type Ia Supernova + +?? (single degenerate)?

More information

2 X-ray 6 gamma-ray 7 1 17.1 0:38m 0:77m nm 17.2 Hz Hz 1 E p E E = h = ch= (17.2) p = E=c = h=c = h= (17.3) continuum continuous spectrum line spectru

2 X-ray 6 gamma-ray 7 1 17.1 0:38m 0:77m nm 17.2 Hz Hz 1 E p E E = h = ch= (17.2) p = E=c = h=c = h= (17.3) continuum continuous spectrum line spectru 1 17 object 1 observation 17.1 X electromagnetic wave photon 1 = c (17.1) c =3 10 8 ms ;1 m mm = 10 ;3 m m =10 ;6 m nm = 10 ;9 m 1 Hz 17.1 spectrum radio 2 infrared 3 visual light optical light 4 ultraviolet

More information

スライド 1

スライド 1 2004/12/25 HOP JTPF JASMINE ILOM JAXA) SPICA JELT Yerkes 1m (1897) Palomar 5m (1948) Subaru 8m (1999) 6.5m Large Binocular Telescope(LBT) 8.4m Mt.Graham 18 3m-6m 6.5m 3m Hubble Space Telescope 2.4m (0.115

More information

3 6 6.1: ALMA 6.1 galaxy, galaxies the Galaxy, our Galaxy, Milky Way Galaxy G. Galilei W. Herschel cm J.C. Kapteyn H. Sharpley 30 E.P. Hubble 6.2 6.2.1 b l 6.2 b = 0 6.2: l = 0 6.2.2 6.1 6.3 ( 60-100µm)

More information

LAE で探る z~5 での AGN 環境と 周辺銀河へのフィードバック Based on Kikuta et al. in prep. 初代星 初代銀河研究会, Oct 25th Satoshi KIKUTA (SOKENDAI/NAOJ, M2) Collaborators: Masatoshi

LAE で探る z~5 での AGN 環境と 周辺銀河へのフィードバック Based on Kikuta et al. in prep. 初代星 初代銀河研究会, Oct 25th Satoshi KIKUTA (SOKENDAI/NAOJ, M2) Collaborators: Masatoshi LAE で探る z~5 での AGN 環境と 周辺銀河へのフィードバック Based on Kikuta et al. in prep., Oct 25th Satoshi KIKUTA (SOKENDAI/NAOJ, M2) Collaborators: Masatoshi Imanishi, Kazuhiro Shimasaku, Fumiaki Nakata, Yoshiki Matsuoka

More information

ISLE 2010/08/17

ISLE 2010/08/17 ISLE 2010/08/17 Talk plan 1. ISLE 2. 3. 4. 2011A 2010/8/17 OAOUM 2010 ISLE 2010/8/17 OAOUM 2010 ISLE OASIS HAWAII (HgCdTe 1024 1024) 4.2 4.2 arcmin 2, 0.25 arcsec/pix (13 Filters) 2006B FWHM = 0.75 arcsec

More information

2

2 01 02 03 04 05 06 07 08 09 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 2 3 01 02 03 4 04 05 06 5 07 08 09 6 10 11 12 7 13 14 15 8 16 17 18 9 19 20 21 10 22 23 24 11 FIELD MAP 12 13 http://www.pref.ishikawa.jp/shinrin/zei/index.html

More information

ELECTRONIC IMAGING IN ASTRONOMY Detectors and Instrumentation 4 The discovery power of modern astronomoical instruments 5 Instrumentation and dete

ELECTRONIC IMAGING IN ASTRONOMY  Detectors and Instrumentation   4 The discovery power of modern astronomoical instruments  5 Instrumentation and dete ELECTRONIC IMAGING IN ASTRONOMY Detectors and Instrumentation 4 The discovery power of modern astronomoical instruments 5 Instrumentation and detectors 4 2017/4/19 Contents 4.3 Polarization; transverse

More information

宇宙理論研究室ガイダンス

宇宙理論研究室ガイダンス 60 S.L.Glashow Glashow : Interaction Warner Books 4 4 1978 12 CMB 10-40 -40 CMB / The universe in a nutshell A H He C, O Ne, Mg Si Fe Sphere(0.1 cylinder (0. slab (0. Cylinder hole (0. Spherical hole

More information

B

B B07557 0 0 (AGN) AGN AGN X X AGN AGN Geant4 AGN X X X (AGN) AGN AGN X AGN. AGN AGN Seyfert Seyfert Seyfert AGN 94 Carl Seyfert Seyfert Seyfert z < 0. Seyfert I II I 000 km/s 00 km/s II AGN (BLR) (NLR)

More information

110 JAXA JAXA / /

110 JAXA JAXA / / 109 JAXA 4 1 2015 3 31 15 40 27 82 / 7/13 6/2 9/13 22/28 13 8 12 8 8 7 10 9 1 1 21 20 19 17 1988 63 2000 15 5 2 26 5 1 10 0 10 3 8 4 6 4 8 13 2 110 JAXA JAXA 9 12 80 60 40 20 / 50 40 30 20 10 / 0 0 3 18

More information

総研大恒星進化概要.dvi

総研大恒星進化概要.dvi The Structure and Evolution of Stars I. Basic Equations. M r r =4πr2 ρ () P r = GM rρ. r 2 (2) r: M r : P and ρ: G: M r Lagrange r = M r 4πr 2 rho ( ) P = GM r M r 4πr. 4 (2 ) s(ρ, P ) s(ρ, P ) r L r T

More information

( )

( ) 1. 2. 3. 4. 5. ( ) () http://www-astro.physics.ox.ac.uk/~wjs/apm_grey.gif http://antwrp.gsfc.nasa.gov/apod/ap950917.html ( ) SDSS : d 2 r i dt 2 = Gm jr ij j i rij 3 = Newton 3 0.1% 19 20 20 2 ( ) 3 3

More information

global global mass region (matter ) & (I) M3Y semi-microscopic int. Ref.: H. N., P. R. C68, ( 03) N. P. A722, 117c ( 03) Proc. of NENS03 (to be

global global mass region (matter ) & (I) M3Y semi-microscopic int. Ref.: H. N., P. R. C68, ( 03) N. P. A722, 117c ( 03) Proc. of NENS03 (to be Gogny hard core spin-isospin property @ RCNP (Mar. 22 24, 2004) Collaborator: M. Sato (Chiba U, ) ( ) global global mass region (matter ) & (I) M3Y semi-microscopic int. Ref.: H. N., P. R. C68, 014316

More information

Microsoft PowerPoint _nakagawa_kagoshima.ppt [互換モード]

Microsoft PowerPoint _nakagawa_kagoshima.ppt [互換モード] Mira 型変光星プロジェクト現状とKVN の利用 A.Nakagawa, T.Kurayama (Kagoshima University) Mira Project Observation Current Status KVN + VERA 大マゼラン雲 (LMC) のミラ型変光星周期光度関係 実視等級を元に得られた関係 距離に対してLMCの厚みは小さくすべて同じ距離にあるとみなせるため実視等級を利用できる

More information

木曽シュミットによる銀河系最外縁の星生成の観測

木曽シュミットによる銀河系最外縁の星生成の観測 2006 木曽シュミットシンポジウム 上松 木曽シュミットによる 銀河系最外縁の星生成の観測 東大天文センター 小林 尚人 安井 千香子 共同研究者 斎藤正雄 (ALMA 国立天文台 Alan Tokunaga ハワイ大学 内容 1. 銀河系最外縁部 現在の理解 2. Extreme Outer Galaxy Rg>18kpc 研究の意義 3つ 3. Digel Cloud2 best example

More information

pptx

pptx Galactic Archaeology [Fe/H] and [X/Fe] evolve in a galaxy: fossils to tell the evolution history of the galaxy Galactic Archaeology" GRB980425 Hypernovae SN Light Curve & Spectra" bright, broad, blended

More information

1 N Mpc well-defined 1 1) Davis et al. 4)? N 2 CMB COBE CMB 2

1 N Mpc well-defined 1 1) Davis et al. 4)? N 2 CMB COBE CMB 2 Observational Cosmology towards the 21st century Yasushi Suto Department of Physics and Research Center for the Early Universe, University of Tokyo, Tokyo 113-0033 We have witnessed a rapid and significant

More information

Microsoft Word - GPS2017.docx

Microsoft Word - GPS2017.docx Surface elevation changes of Rhonegletscher from 2007 to 2017 Observational report of GPS survey for ten years Ryo Hazuki (1) Yutaka Kurosaki (1) Marie Uemura (1) (1) Graduate School of Environmental Science,

More information

H+He H+He M > 10 M He He Wolf-Rayet Minit = 13 ~ 100 M, Zinit = 0.0001 ~ 0.02 CNO SN 2007bi (Type Ic) progenitor Minit > 100 M, Zinit = 0.004 WO star? Core collapse Rotating star model Saio, Nomoto, and

More information

太陽系外惑星探査

太陽系外惑星探査 http://hubblesite.org/newscenter/archive/2001/38/ Terra MODIS http://modarch.gsfc.nasa.gov/ http://www.nasa.gov/home/index.html / 2 Are we alone? Origins Where are they? (Fermi 1950) 3 4 0.5 arcsec 10pc

More information

1 Radio Astronomy URL AGB dust in galactic environments URL

1 Radio Astronomy URL     AGB dust in galactic environments URL 1 Radio Astronomy URL http://www.hokudai.ac.jp http://www.astro3.sci.hokudai.ac.jp AGB dust in galactic environments 1998 2000 URL http://www.sci.hokudai.ac.jp/ http://www.ep.sci.hokudai.ac.jp/epms/ index.htm

More information

SN 2007bi Yoshida, T. & Umeda, H., MNRAS 412, L78-L82 (2011)

SN 2007bi Yoshida, T. & Umeda, H., MNRAS 412, L78-L82 (2011) SN 2007bi Yoshida, T. & Umeda, H., MNRAS 412, L78-L82 (2011) SN 2007bi SN 2007bi (Gal-Yam et al. 2009) 2007 4 6.5 Type Ic subluminous dwarf galaxy Z ~ (0.2-0.4) Z (Young et al. 2010) 36 (Young et al. 2010)

More information

PowerPoint プレゼンテーション

PowerPoint プレゼンテーション HSC-SSP 1 2016.4.11 HSC DB 2 HSC 2012/8 FL 2014/3 SSP 7 104 Suprime-Cam HSC : 27 34 10 2k4k CCDs : 1.5 104 2k4k CCDs : 185MB/shot 30GB/ 2GB/shot ( 300GB/ ) : 1 10 1400 1. CCD 2. CCD 3. 4. CCD 4 K -IPMU

More information

0.45m1.00m 1.00m 1.00m 0.33m 0.33m 0.33m 0.45m 1.00m 2

0.45m1.00m 1.00m 1.00m 0.33m 0.33m 0.33m 0.45m 1.00m 2 24 11 10 24 12 10 30 1 0.45m1.00m 1.00m 1.00m 0.33m 0.33m 0.33m 0.45m 1.00m 2 23% 29% 71% 67% 6% 4% n=1525 n=1137 6% +6% -4% -2% 21% 30% 5% 35% 6% 6% 11% 40% 37% 36 172 166 371 213 226 177 54 382 704 216

More information

10 117 5 1 121841 4 15 12 7 27 12 6 31856 8 21 1983-2 - 321899 12 21656 2 45 9 2 131816 4 91812 11 20 1887 461971 11 3 2 161703 11 13 98 3 16201700-3 - 2 35 6 7 8 9 12 13 12 481973 12 2 571982 161703 11

More information

Summary of WISH Filter Set and Sensitivity: Filters suitable for various scientific case Filters cover wavelength range of 1-5µm without any gaps Narr

Summary of WISH Filter Set and Sensitivity: Filters suitable for various scientific case Filters cover wavelength range of 1-5µm without any gaps Narr Summary of WISH Survey Plan Kiyoto Yabe (NAOJ) Summary of WISH Filter Set and Sensitivity: Filters suitable for various scientific case Filters cover wavelength range of 1-5µm without any gaps Narrower

More information

07.報文_及川ら-二校目.indd

07.報文_及川ら-二校目.indd 8 01 01 4 4 1 5 16 18 6 006 H 18 4 011 H 6 4 1 5 1 5 007 H 19 5 009 1 5 006 007 009 011 9 10 4 000 H 1 4 5 004 H 16 4 004 009 H 1 5 4 4 5 1 4 006 011 1 1 4m 5m 10m 007 1 7 009 009 1 5 10 1 000kg 10a 006

More information

atomic line spectrum emission line absorption line atom proton neutron nuclei electron Z atomic number A mass number neutral atom ion energy

atomic line spectrum emission line absorption line atom proton neutron nuclei electron Z atomic number A mass number neutral atom ion energy 1 22 22.1 atomic line spectrum emission line absorption line atom proton neutronnuclei electron Z atomic number A mass number neutral atom ion energy level ground stateexcited state ionized state 22.2

More information

PowerPoint プレゼンテーション

PowerPoint プレゼンテーション 弱い重力レンズの宇宙論と重力理論の 検証への応用 二間瀬敏史 理学部 22 May. 2017 内容 弱い重力レンズの紹介 構造形成理論への応用 Verlinde s Emergent Gravity の検証 超新星のm-z 関係とニュートリノ質量 重力レンズとは? 観測者 銀河団 背景銀河 J-P.Kneib. Ph.D thesis なぜ重力レンズが重要なのか? 直接的な質量検出 重力のみに依存し

More information

dark matter density profiles

dark matter density profiles LSS & CDM 2 LSS & CDM 3 SPH simulation: movie SPH simulation in CDM : dark matter hot gas galaxy (Yoshikawa, Taruya, Jing & Suto 2001) LSS & CDM 4 Confronting elements of the CDM paradigm Global cosmological

More information

PowerPoint Presentation

PowerPoint Presentation Sgr A* の赤外線観測 西山正吾 ( 京都大学 ) NIR obserbvations of the Galactic center 2/46 NIR obserbvations of the Galactic center 3/46 NIR obserbvations of the Galactic center 4/46 Dereddened flux density [mjy] 40 20

More information

2007/8 Vol. J90 D No. 8 Stauffer [7] 2 2 I 1 I 2 2 (I 1(x),I 2(x)) 2 [13] I 2 = CI 1 (C >0) (I 1,I 2) (I 1,I 2) Field Monitoring Server

2007/8 Vol. J90 D No. 8 Stauffer [7] 2 2 I 1 I 2 2 (I 1(x),I 2(x)) 2 [13] I 2 = CI 1 (C >0) (I 1,I 2) (I 1,I 2) Field Monitoring Server a) Change Detection Using Joint Intensity Histogram Yasuyo KITA a) 2 (0 255) (I 1 (x),i 2 (x)) I 2 = CI 1 (C>0) (I 1,I 2 ) (I 1,I 2 ) 2 1. [1] 2 [2] [3] [5] [6] [8] Intelligent Systems Research Institute,

More information

030801調査結果速報版.PDF

030801調査結果速報版.PDF 15 8 1 15 7 26 1. 2. 15 7 27 15 7 28 1 2 7:13 16:56 0:13 3km 45 346 108 3.1 3.2 3.3 3.4 3.5 3.6 3.7 3.8 3.9 3.10 3.11 3. 3.1 26 7 10 1 20cm 2 1 2 45 1/15 3 4 5,6 3 4 3 5 6 ( ) 7,8 8 7 8 2 55 9 10 9 10

More information

宇宙ガンマ線観測で解き明かす暗黒物

宇宙ガンマ線観測で解き明かす暗黒物 2/30 72% 5% 23% ~1 3/30 Matthew Newby, Milkyway@home mv 2 r v = = GmM(r) r 2 GM(r) r (km/s) (AU) 4/30 5/30 Mark Whittle, University of Virginia Department of Astronomy Adam Block/Mount Lemmon SkyCenter/University

More information

理論懇2014

理論懇2014 Proposal for a project of high-precision stellar radial velocity work, Struve (1952)! But there seems to be no compelling reason why the hypothetical stellar planets should not, in some instances, be much

More information

系外惑星大気

系外惑星大気 http://hubblesite.org/newscenter/archive/2001/38/ 2004 9 30 1781 1846 1930 50 2 3 radial velocity HDS 5m/s HD209458 HD209458+I 2 cell Subaru/HDS 4 (Mayor & Queloz 1995) 4.2 5 2 1.5% HST 4 orbits Brown

More information

3

3 3 Introduction... Ceres, Juno, Vesta, Ida, Mathilde, Eros, Gaspra, Itokawa Ceres Juno, Vesta, Ida, Eros, Gaspra. Surface Color Variation of Ida and Vesta Ida: 48-49 37-40 352-355 337-341 307-311 277-280

More information

撮 影

撮 影 DC cathode ray tube, 2.2 log log log + log log / / / A method determining tone conversion characteristics of digital still camera from two pictorial images Tone conversion characteristic Luminance

More information

HSC NB515 9 28 ( ) FD PBL HSC NB515 NB515 NB515 Ferguson+02 Tanaka+10 ~8Gyr Brown+03 Tanaka+10 20kpc de Vaucouleurs (r 1/4 ) Irwin+05,Tanaka+10, metal thick disk thin disk 70kpc Ibata+05 Guhathakurta+05,

More information

10 0 10-1 100 Mpc simulation (z = 1.0) 34 Mpc simulation (z = 1.0) (Mpc/h) -3 / mag 10-2 10-3 10-4 10-5 -24-22 -20-18 -16-14 M B - 5 log h (Mpc/h) -3 / mag 10 0 10-1 10-2 10-3 10-4 conbined simulation

More information

PowerPoint Presentation

PowerPoint Presentation 2010 KEK (Japan) (Japan) (Japan) Cheoun, Myun -ki Soongsil (Korea) Ryu,, Chung-Yoe Soongsil (Korea) 1. S.Reddy, M.Prakash and J.M. Lattimer, P.R.D58 #013009 (1998) Magnetar : ~ 10 15 G ~ 10 17 19 G (?)

More information

Akira MIZUTA(KEK) AM, Nagataki, Aoi (ApJ, , 2011) AM + (in prep)

Akira MIZUTA(KEK) AM, Nagataki, Aoi (ApJ, , 2011) AM + (in prep) Akira MIZUTA(KEK) AM, Nagataki, Aoi (ApJ, 732 26, 2011) AM + (in prep) 2011.12.28 GRB GRB. ex. GRB980425/SN1998bw, GRB030329/SN2003dh XRF060218/SN2006aj. GRB091127/SN2009nz XRF100316D/SN2010bh Spectrum

More information

( ) 2 self-consistent 1 3) ( ) 2.1 ( ) ( 1 kpc 10 8 M 10 4 K) 1024 2 4096 2 100 1680 ( 1) 10 K 10 4 5 K tangled-web model ( ) 2

( ) 2 self-consistent 1 3) ( ) 2.1 ( ) ( 1 kpc 10 8 M 10 4 K) 1024 2 4096 2 100 1680 ( 1) 10 K 10 4 5 K tangled-web model ( ) 2 Numerical Modeling of the Interstellar Medium WADA Keiichi (National Astronomical Observatory of Japan) Abstract The interstellar medium in galaxies has a complicated multi-phase structure. However, in

More information

1 Credit: NASA/JPL-Caltech/R. Hurt SSC-Caltech ,

1 Credit: NASA/JPL-Caltech/R. Hurt SSC-Caltech , 397 0101 10762 30 e-mail: matsunaga@ioa.s.u-tokyo.ac.jp 8 3 20 2 3 3 7 2 3 1. 100 1912 1 1 4 12 10 3 1 20 2,500 2 1 3 4 374 2012 6 1 Credit: NASA/JPL-Caltech/R. Hurt SSC-Caltech 3 2. 5 3 6 100 7 8, 9 10

More information

42 1 Fig. 2. Li 2 B 4 O 7 crystals with 3inches and 4inches in diameter. Fig. 4. Transmission curve of Li 2 B 4 O 7 crystal. Fig. 5. Refractive index

42 1 Fig. 2. Li 2 B 4 O 7 crystals with 3inches and 4inches in diameter. Fig. 4. Transmission curve of Li 2 B 4 O 7 crystal. Fig. 5. Refractive index MEMOIRS OF SHONAN INSTITUTE OF TECHNOLOGY Vol. 42, No. 1, 2008 Li 2 B 4 O 7 (LBO) *, ** * ** ** Optical Scatterer and Crystal Growth Technology of LBO Single Crystal For Development with Optical Application

More information

214 1 11 SU UMa AY Lyr AY ASASSN-14jv CCD ASASSN-14jv SU UMa WZ Sge 28 29 AY Lyr O-C

214 1 11 SU UMa AY Lyr AY ASASSN-14jv CCD ASASSN-14jv SU UMa WZ Sge 28 29 AY Lyr O-C AY Lyr ASASSN-14jv CCD I11G22 214 1 11 SU UMa AY Lyr AY ASASSN-14jv CCD ASASSN-14jv SU UMa WZ Sge 28 29 AY Lyr O-C 1 4 1.1............................. 4 1.2................................ 5 2 7 3 9 4

More information

II (No.2) 2 4,.. (1) (cm) (2) (cm) , (

II (No.2) 2 4,.. (1) (cm) (2) (cm) , ( II (No.1) 1 x 1, x 2,..., x µ = 1 V = 1 k=1 x k (x k µ) 2 k=1 σ = V. V = σ 2 = 1 x 2 k µ 2 k=1 1 µ, V σ. (1) 4, 7, 3, 1, 9, 6 (2) 14, 17, 13, 11, 19, 16 (3) 12, 21, 9, 3, 27, 18 (4) 27.2, 29.3, 29.1, 26.0,

More information

Contents 1. Ia cosmology 2. Ia / rate 3.

Contents 1. Ia cosmology 2. Ia / rate 3. WISH ( ) Contents 1. Ia cosmology 2. Ia / rate 3. supernova (CC SN) Ia (SN Ia) supernova classification supernova Ia (SN Ia) - : redshift z~1.5 - progenitor system: Single Degenerate? Double Degenerate?

More information

第43回夏の学校2013(馬場).key

第43回夏の学校2013(馬場).key 渦状腕の正体 発生 維持メカニズムは -どのように回転しているか -持続時間はどのくらいか -渦状腕の本数は何で決まるのか (多様性の起源)...etc. M83 棒状構造 M74 Grand-Design型渦状腕 M101 Multi-Arm型渦状腕 2 M63 Flocculent型渦状腕 1964ApJ...140..646L 渦状腕論争(1960 s ) 渦状腕 = 実体 or 準定常波 Lin

More information

Takeshi Kudo 1, Yukihiro Takahashi 1, Mitsuteru Sato 1, Taishi Yamada 1, Nui Kobayashi 1, Yusuke Sanmiya 1, Tomohiro Inoue 2, H C Stenbaek- Nielsen 3,

Takeshi Kudo 1, Yukihiro Takahashi 1, Mitsuteru Sato 1, Taishi Yamada 1, Nui Kobayashi 1, Yusuke Sanmiya 1, Tomohiro Inoue 2, H C Stenbaek- Nielsen 3, Takeshi Kudo 1, Yukihiro Takahashi 1, Mitsuteru Sato 1, Taishi Yamada 1, Nui Kobayashi 1, Yusuke Sanmiya 1, Tomohiro Inoue 2, H C Stenbaek- Nielsen 3, Ma@hew G McHarg 4, Ryan K Haaland 5, Takeshi Kammae

More information

2 g g = GM R 2 = 980 cm s ;1 M m potential energy E r E = ; GMm r (1.4) potential = E m = ;GM r (1.5) r F E F = ; de dr (1.6) g g = ; d dr (1.7) g g g

2 g g = GM R 2 = 980 cm s ;1 M m potential energy E r E = ; GMm r (1.4) potential = E m = ;GM r (1.5) r F E F = ; de dr (1.6) g g = ; d dr (1.7) g g g 1 1 (gravitation) 1.1 m F a ma = F (1.1) F a m F 1.1 m F a (1.1) m a F m F a m a F F a m 0 0 1.2 (universal gravitation) (potential) M m gravitational force F r F = ; GMm r 2 (1.2) G = 6:67 10 ;8 dyn cm

More information

4 19

4 19 I / 19 8 1 4 19 : : f(e, J), f(e) Phase mixing Landau Damping, violent relaxation : 2 2 : ( ) http://antwrp.gsfc.nasa.gov/apod/ap950917.html ( ) http://www-astro.physics.ox.ac.uk/~wjs/apm_grey.gif

More information

Formation process of regular satellites on the circumplanetary disk Hidetaka Okada Department of Earth Sciences, Undergraduate school of Scie

Formation process of regular satellites on the circumplanetary disk Hidetaka Okada Department of Earth Sciences, Undergraduate school of Scie Formation process of regular satellites on the circumplanetary disk Hidetaka Okada 22060172 Department of Earth Sciences, Undergraduate school of Science, Hokkaido University Planetary and Space Group

More information

cm H.11.3 P.13 2 3-106-

cm H.11.3 P.13 2 3-106- H11.3 H.11.3 P.4-105- cm H.11.3 P.13 2 3-106- 2 H.11.3 P.47 H.11.3 P.27 i vl1 vl2-107- 3 h vl l1 l2 1 2 0 ii H.11.3 P.49 2 iii i 2 vl1 vl2-108- H.11.3 P.50 ii 2 H.11.3 P.52 cm -109- H.11.3 P.44 S S H.11.3

More information

kawaguchi2.pdf

kawaguchi2.pdf Dusty Clumpy Torus (AGN) (BH) BH 3 BH 1 AGN () 1/3 (i) (ii) Kawaguchi(2003) 1/5 (iii) AGN : T. Kawaguchi & M. Mori, ApJL, 2010, 724, 183 187 T. Kawaguchi & M. Mori, ApJ, 2011, 737, 105 120 Toshihiro KAWAGUCHI

More information

SFN saigo

SFN saigo 2017年10月20日 西合 SFN 296 #36 Chandra X-ray observation of the young stellar cluster NGC 3293 in the Carina Nebula Complex T. Preibisch, S. Flaischlen, B. Gaczkowski, L. Townsley and P. Broos Accepted by

More information

X u

X u X u1079037 14 4 1 X X X X X SNR X X ChandraX 0.3-10.0 kev 1 1 X 3 X 1 3 2 X 5 2.1 X... 5 2.1.1 Powerlaw... 5 2.1.2 BlackBody( )... 5 2.1.3 Disk-BlackBody... 6 2.1.4... 8 2.2 X... 9 2.2.1 HMXB:High-Mass

More information

Isogai, T., Building a dynamic correlation network for fat-tailed financial asset returns, Applied Network Science (7):-24, 206,

Isogai, T., Building a dynamic correlation network for fat-tailed financial asset returns, Applied Network Science (7):-24, 206, H28. (TMU) 206 8 29 / 34 2 3 4 5 6 Isogai, T., Building a dynamic correlation network for fat-tailed financial asset returns, Applied Network Science (7):-24, 206, http://link.springer.com/article/0.007/s409-06-0008-x

More information

1 1.1,,,.. (, ),..,. (Fig. 1.1). Macro theory (e.g. Continuum mechanics) Consideration under the simple concept (e.g. ionic radius, bond valence) Stru

1 1.1,,,.. (, ),..,. (Fig. 1.1). Macro theory (e.g. Continuum mechanics) Consideration under the simple concept (e.g. ionic radius, bond valence) Stru 1. 1-1. 1-. 1-3.. MD -1. -. -3. MD 1 1 1.1,,,.. (, ),..,. (Fig. 1.1). Macro theory (e.g. Continuum mechanics) Consideration under the simple concept (e.g. ionic radius, bond valence) Structural relaxation

More information

銀河団衝突にともなう 高温ガスの運動がひきおこす特徴的な磁場構造 (Takizawa 2008 ApJ, 687, 951)

銀河団衝突にともなう 高温ガスの運動がひきおこす特徴的な磁場構造 (Takizawa 2008 ApJ, 687, 951) JVLA S-band and X-band Polarimetry of Abell 2256 Ozawa,,,,,Takizawa, Takahashi,,,,et al. to be submitted to PASJ 滝沢元和 2015.5.8 研究室談話会 Introduction: 銀河団 可視光 ( 数 100 個の銀河の集まり ) X 線数 kev の高温ガス ( シンクロトロン )

More information

スライド 1

スライド 1 精度銀河形成 シミュレーション時代の幕開け 斎藤貴之国 天 台天 シミュレーションプロジェクト 共同研究者松井秀典 久保英 郎 和 桂 富阪幸治 牧野淳 郎 (NAOJ) 台坂博 ( 橋 ) 吉 直紀 ( 東 ) 岡本崇 ( 筑波 ) 場淳 ( 東北 ) 初期条件 我々の宇宙がどのような進化をするかは極めて正確にわかっている 冷たい暗 物質が 配する宇宙 宇宙背景放射 銀河サーベイなどの結果から さな構造が先にでき

More information

Microsoft PowerPoint - ICRRseminar_AkariSpica_ pptx

Microsoft PowerPoint - ICRRseminar_AkariSpica_ pptx SPICA 2010 7 16 ICRR ISAS,JAXA List of my talk Bright Source Catalog Science Highlights Warm Mission SPICA 2 地球大気の透過率 & 放射強度 3 地球大気の吸収を逃れる 地球大気の放射から逃れる なぜ宇宙へ? 4,000m 級の高山に上っても 大気の赤外線放射は 宇宙から来る赤外線の 100

More information

vol5-honma (LSR: Local Standard of Rest) 2.1 LSR R 0 LSR Θ 0 (Galactic Constant) 1985 (IAU: International Astronomical Union) R 0 =8.5

vol5-honma (LSR: Local Standard of Rest) 2.1 LSR R 0 LSR Θ 0 (Galactic Constant) 1985 (IAU: International Astronomical Union) R 0 =8.5 2.2 1 2.2 2.2.1 (LSR: Local Standard of Rest) 2.1 LSR R 0 LSR Θ 0 (Galactic Constant) 1985 (IAU: International Astronomical Union) R 0 =8.5 kpc, Θ 0 = 220 km s 1. (2.1) R 0 7kpc 8kpc Θ 0 180 km s 1 270

More information

Mathews Grant J. (University of Notre Dame) Boyd Richard N. (Lawrence Livermore National Laboratory) 2009/5/21

Mathews Grant J. (University of Notre Dame) Boyd Richard N. (Lawrence Livermore National Laboratory) 2009/5/21 Mathews Grant J. (University of Notre Dame) Boyd Richard N. (Lawrence Livermore National Laboratory) 2009/5/21 Abstract strongly interacting massive particles (SIMPs, X) Big Bang (BBN) X heavy colored

More information

2 Windows 10 *1 3 Linux 3.1 Windows Bash on Ubuntu on Windows cygwin MacOS Linux OS Ubuntu OS Linux OS 1 GUI Windows Explorer Mac Finder 1 GUI

2 Windows 10 *1 3 Linux 3.1 Windows Bash on Ubuntu on Windows cygwin MacOS Linux OS Ubuntu OS Linux OS 1 GUI Windows Explorer Mac Finder 1 GUI 2017 1 2017 -September I ll remember- 1,2 Linux 6 Linux Linux 2 3 Linux 2 (OS) Windows MacOS OS MacOS Linux 3 Windows Windows ( ) 1. Bash on Ubuntu on Windows ( Windows 10 ) 2. cygwin ( ) 3. VM Ware Linux

More information

ΤΕΙ Ιονίων Νήσων - Εργαστηριακές Ασκήσεις στα Γεωγραφικά Συστήματα Πληροφοριών

ΤΕΙ Ιονίων Νήσων - Εργαστηριακές Ασκήσεις στα Γεωγραφικά Συστήματα Πληροφοριών 1 71 71 71 71 71 71 71 71 71 71 73 1 71 7 1 71 71 71 71 71 71 71 7):1 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 71 7-1 71 71 71 71 71 71 71 71 71 71 71 71 71

More information

Microsoft Word - mitomi_v06.doc

Microsoft Word - mitomi_v06.doc MSS mitomi@edm.bosai.go.jp matsuoka@edm.bosai.go.jp yamazaki@edm.bosai.go.jp taniguchi@manage.nitech.ac.jp 1 MSS MSS 2 2 1 m MSS CCT CCT Fig.1 CCT b02-b0 b0-b0b-b b-b1 CCT Landsat/TM MSS S/N 21x21 21x21

More information

dTVIIman.PDF

dTVIIman.PDF dtv.ii SR diffusion TENSOR Visualizer II, the Second Release Rev.0.90 (2005.08.22) dtv 3 6 ROI ROI 10 11 15 21 23 25 2 dtv dtvdiffusion TENSOR Visualizer MR VOLUME-ONE dtv VOLUME-ONE ROI 1.1 dtv.ii SR

More information

50cm

50cm 50cm 2005 2 Abstract Gamma-ray bursts (GRBs) are the largest explosions at large distances. The purpose of our study is to observe GRBs and their afterglows to investigate the physical mechanism of GRBs.

More information

4/15 No.

4/15 No. 4/15 No. 1 4/15 No. 4/15 No. 3 Particle of mass m moving in a potential V(r) V(r) m i ψ t = m ψ(r,t)+v(r)ψ(r,t) ψ(r,t) = ϕ(r)e iωt ψ(r,t) Wave function steady state m ϕ(r)+v(r)ϕ(r) = εϕ(r) Eigenvalue problem

More information

森羅万象2018のコピー

森羅万象2018のコピー PD Stellar Irradiation Mineral Atmosphere Na, K, SiO, O 2, O gas (MgO, Al, AlO, FeO etc ) https://www.nasa.gov/topics/universe/features/rocky_planet.html / (2018.5.9) Magma Ocean Ito et al. (2015) (HRE)

More information

: 8.2: A group (i.e. a very small cluster) of galaxies superimposed on a x-ray image from the ROSAT satellite

: 8.2: A group (i.e. a very small cluster) of galaxies superimposed on a x-ray image from the ROSAT satellite 1 8 8.1 8.1.1 8.1: ( Ω = ρ/ρ c ) (Fukugita, M. et al., APJ 503 (1998) 518) ( 15%) (z 0 ) 1.................. 0.0026 h 1 0.0043 h 1 0.0014 h 1 A 2..................... 0.00086 h 1 0.00129 h 1 0.00051 h

More information

パナソニック技報

パナソニック技報 Liquid Crystal Display Technology for Realizing Contrast Ratio of 1 million to 1 Katsuhiro Kikuchi LCDLiquid Crystal Display IPSIn-Plane Switching-LCD 2100:1 IPS-LCDIPS-LCD50 20:1 Realization of Liquid

More information

系外惑星大気

系外惑星大気 transiting planet http://hubblesite.org/newscenter/archive/2001/38/ 2004 6 17 HDS 2 3 (Mayor & Queloz 1995) 4.2 4 (Charbonneau et al. 2000, Henry et al. 2000) HST HST Brown et al. (2001) 5 6 Radial velocity

More information

[1] 2 キトラ古墳天文図に関する従来の研究とその問題点 mm 3 9 mm cm 40.3 cm 60.6 cm 40.5 cm [2] 9 mm [3,4,5] [5] 1998

[1] 2 キトラ古墳天文図に関する従来の研究とその問題点 mm 3 9 mm cm 40.3 cm 60.6 cm 40.5 cm [2] 9 mm [3,4,5] [5] 1998 18 1 12 2016 キトラ古墳天文図の観測年代と観測地の推定 2015 5 15 2015 10 7 Estimating the Year and Place of Observations for the Celestial Map in the Kitora Tumulus Mitsuru SÔMA Abstract Kitora Tumulus, located in Asuka, Nara

More information

大学通信vol199

大学通信vol199 199 16. 17. 2. 3. 12. 4. 6. 18. 14. 8. 11. 13. 21. 20. 22. 23. Club 3 4 2014 2 AICHI UNIVERSITY 3 4 AICHI UNIVERSITY 5 6 AICHI UNIVERSITY 7 action A NOW 8 action A AICHI UNIVERSITY 9 action A 10 AICHI

More information

Vol. 44 No. SIG 9(CVIM 7) ) 2) 1) 1 2) 3 7) 1) 2) 3 3) 4) 5) (a) (d) (g) (b) (e) (h) No Convergence? End (f) (c) Yes * ** * ** 1

Vol. 44 No. SIG 9(CVIM 7) ) 2) 1) 1 2) 3 7) 1) 2) 3 3) 4) 5) (a) (d) (g) (b) (e) (h) No Convergence? End (f) (c) Yes * ** * ** 1 Vol. 44 No. SIG 9(CVIM 7) July 2003, Robby T. Tan, 1 Estimating Illumination Position, Color and Surface Reflectance Properties from a Single Image Kenji Hara,, Robby T. Tan, Ko Nishino, Atsushi Nakazawa,

More information

02-量子力学の復習

02-量子力学の復習 4/17 No. 1 4/17 No. 2 4/17 No. 3 Particle of mass m moving in a potential V(r) V(r) m i ψ t = 2 2m 2 ψ(r,t)+v(r)ψ(r,t) ψ(r,t) Wave function ψ(r,t) = ϕ(r)e iωt steady state 2 2m 2 ϕ(r)+v(r)ϕ(r) = εϕ(r)

More information

Gravothermal Catastrophe & Quasi-equilibrium Structure in N-body Systems

Gravothermal Catastrophe & Quasi-equilibrium Structure  in N-body Systems 2004/3/1 3 N 1 Antonov Problem & Quasi-equilibrium State in N-body N Systems A. Taruya (RESCEU, Univ.Tokyo) M. Sakagami (Kyoto Univ.) 2 Antonov problem N-body study of quasi-attractivity M15 T Antonov

More information

Atmospheric gas dynamics in the Perseus cluster observed with Hitomi

Atmospheric gas dynamics in the Perseus cluster  observed with Hitomi Atmospheric gas dynamics in the Perseus cluster observed with Hitomi Hitomi collaboration Shutaro Ueda, Yuto Ichinohe Ryuichi Fujimoto, Shota Inoue, Caroline Kilbourne, Tetsu Kitayama, Maxim Markevitch,

More information

塗装深み感の要因解析

塗装深み感の要因解析 17 Analysis of Factors for Paint Depth Feeling Takashi Wada, Mikiko Kawasumi, Taka-aki Suzuki ( ) ( ) ( ) The appearance and quality of objects are controlled by paint coatings on the surfaces of the objects.

More information

A 99% MS-Free Presentation

A 99% MS-Free Presentation A 99% MS-Free Presentation 2 Galactic Dynamics (Binney & Tremaine 1987, 2008) Dynamics of Galaxies (Bertin 2000) Dynamical Evolution of Globular Clusters (Spitzer 1987) The Gravitational Million-Body Problem

More information

"Moir6 Patterns on Video Pictures Taken by Solid State Image Sensors" by Okio Yoshida and Akito Iwamoto (Toshiba Research and Development Center, Tosh

Moir6 Patterns on Video Pictures Taken by Solid State Image Sensors by Okio Yoshida and Akito Iwamoto (Toshiba Research and Development Center, Tosh "Moir6 Patterns on Video Pictures Taken by Solid State Image Sensors" by Okio Yoshida and Akito Iwamoto (Toshiba Research and Development Center, Toshiba Corporation, Kawasaki) Reproduced resolution chart

More information

Λ (Λ ) Λ (Ge) Hyperball γ ΛN J-PARC Λ dead time J-PARC flash ADC 1 dead time ( ) 1 µsec 3

Λ (Λ ) Λ (Ge) Hyperball γ ΛN J-PARC Λ dead time J-PARC flash ADC 1 dead time ( ) 1 µsec 3 19 Λ (Λ ) Λ (Ge) Hyperball γ ΛN J-PARC Λ dead time J-PARC flash ADC 1 dead time ( ) 1 µsec 3 1 1 1.1 γ ΛN................. 1 1.2 KEK J-PARC................................ 2 1.2.1 J-PARC....................................

More information

1 Kinect for Windows M = [X Y Z] T M = [X Y Z ] T f (u,v) w 3.2 [11] [7] u = f X +u Z 0 δ u (X,Y,Z ) (5) v = f Y Z +v 0 δ v (X,Y,Z ) (6) w = Z +

1 Kinect for Windows M = [X Y Z] T M = [X Y Z ] T f (u,v) w 3.2 [11] [7] u = f X +u Z 0 δ u (X,Y,Z ) (5) v = f Y Z +v 0 δ v (X,Y,Z ) (6) w = Z + 3 3D 1,a) 1 1 Kinect (X, Y) 3D 3D 1. 2010 Microsoft Kinect for Windows SDK( (Kinect) SDK ) 3D [1], [2] [3] [4] [5] [10] 30fps [10] 3 Kinect 3 Kinect Kinect for Windows SDK 3 Microsoft 3 Kinect for Windows

More information

Sample function Re random process Flutter, Galloping, etc. ensemble (mean value) N 1 µ = lim xk( t1) N k = 1 N autocorrelation function N 1 R( t1, t1

Sample function Re random process Flutter, Galloping, etc. ensemble (mean value) N 1 µ = lim xk( t1) N k = 1 N autocorrelation function N 1 R( t1, t1 Sample function Re random process Flutter, Galloping, etc. ensemble (mean value) µ = lim xk( k = autocorrelation function R( t, t + τ) = lim ( ) ( + τ) xk t xk t k = V p o o R p o, o V S M R realization

More information

56cm 1 15 1960 2 8 2 2 1 2008 1992 2 1992 2 3562mm 3773mm 2 1980 1991 2008 2007 2003 5 2 3 2003 2005 2008 2010 2005 2008 2012 2010 2012 4 7 4 5 2 1975 1994 8 2008 NPO 2 2010 3 2013 2016 3 2008 2009 14

More information

KT Eridani I08GM01/

KT Eridani I08GM01/ KT Eridani I8GM1/ 21 2 1 Abstract KT Eridani(Nova Eridani 29) 29 11 255 (UT) 81 11 26 (R 4) (lter: B, V, y, Rc) 11 26 He I, N II, N III Hα FWHM 34km/s He/N nova 148 (GSC53251837) ASAS Pi of the sky 11

More information