观测宇宙学的一些新进展.ppt

观测宇宙学的一些新进展北京师范大学天文系何香涛 陈阳大爆炸宇宙的提出和标准化l1927年，勒梅特，“原始光子”l1948年，伽莫夫(Gamov)、阿尔芬(Alpher)、 贝色(Bethe)，--理论l1957年，B2FH（G.Burbidge,F.Burbidge,Fowler and Hoyle) l1965年，宇宙微波背景发现标准化进程：爱因斯坦，弗里德曼，罗伯逊，沃克，勒梅特，伽莫夫热大爆炸宇宙模型－标准宇宙模型宇宙中的物质分布是均匀和各项同性的目前的宇宙处于膨胀状态宇宙起源于一次热大爆炸宇宙时空用R－W度规来描述从热大爆炸宇宙诞生l光子粒子对lTKB＝2mc2lT2mc2/KB3分钟造就一个宇宙最初三分钟lT＝1013 核子：质子，反质子，中子，反中子t＝1.510-6秒lT＝1012 强子： 介子 t＝1.210-4秒lT＝1011 光子和粒子热动平衡 t＝0.01秒lT＝1010 中微子逃逸 t＝1.1秒lT＝109 正负电子湮灭，电子、质子、氘和氦 t＝3分45秒宇宙的极早期<10-6秒，物质和辐射不可分，引力可能量子化 一片夸克海洋人的认识极限－量子化• ⊿E⊿t ≈ ћћ=h/2，h=6.62510-27erg · s•产生粒子对 ⊿E＝2mc2 的时间⊿t ＝tc＝ћ/2mc2 ---康普顿时间•光穿过一个m基本粒子的时间ts＝2Gm/c3 ---史瓦西时间极限物理量l令tc＝ts，普朗克质量 普朗克时间普朗克长度 普朗克温度 T=1032K 支持热大爆炸的主要观测事实∆目前的宇宙在膨胀着∆存在着各向同性的黑体谱宇宙背景辐射∆氦和氘的宇宙丰度（约占1/4）必须借助早期的宇宙核合成∆宇宙的年龄不超过200亿年观测能力极大提高 －多波段天文学γ-rayX－ray光学红外射电X－ray 巡天Uhuru（自由号） 1970 HERO－1 高能天文台 1977 HERO－2 爱因斯坦天文台 1978 HERO－3 1979 白鸟 (Hakucho) 1979 天马 (Tenma － Astro-B) 1983 EXOSAT 1983 银河 (Ginga － Astro-C) 1987ROSAT 1990 ASCA (Astro-D) 1993－2001BeppoSAX 1996－2002RXTE 1995－(ROSS X-ray Timing Explorer)Chandra (AXAF) 1999 (NASA)XMM-Newton 1999The Uhuru SatelliteThe HEAO-1 Satellite The HEAO-3 Satellite The Einstein Observatory (HEAO-2) The Hakucho SatelliteThe Tenma [Astro B] SatelliteThe EXOSAT ObservatoryThe Ginga SatelliteASCA: The Advanced Satellite for Cosmology and AstrophysicsBeppoSAXThe Rossi X-rayTiming ExplorerROSAT : The Roentgen Satellite Chandra X-ray Observatory Mission ChandraLifetime : 23 July 1999 - (nominal 5 year mission) ØEnergy Range : 0.1-10 keV ØSpecial Features : 64 Hours highly-eccentric Earth orbit.Spatial resolution < 1 arcsec lScience Hightlight: ØX-ray imaging the sources associated with Gamma-ray bursts and determining their positions with an unprecedented precision. ØMonitoring the X-ray afterglow of Gamma-ray bursts The X-ray Multi-Mirror Mission (XMM-Newton)Mission XMM-Newtonl Lifetime : December 1999 - (nominal 10 year mission) l Energy Range : 0.1-15 keV l Special Features : Very large collecting area. Simulataneous X-ray & Optical observations. The following figure compares the XMM-Newton mirror areas with those of other recent X-ray observatories (note that the detector efficiency has not been included). The figure clearly shows the greater area and extended energy range of XMM-Newton compared to ROSAT, ASCA, and even Chandra.光 学 巡 天巡天极限星等发现天体 Markarian15.m5~500 Kiso（木曾）~19.m0~10,000 Palomar BQS16.m2~100 LBQS~18.m51054 Edinburgh/Cape~17.m0240 HST WF/PC~28.m0~3000 SDSS~20.m0~1052dFDeep Extragalactic Evolutionary Probe ( DEEP )The Deep Extragalactic Evolutionary Probe (DEEP) is a multi-year program which uses the twin 10-m Keck Telescopes and the Hubble Space Telescope to conduct a large scale survey of distant, faint, field galaxies. 红 外 巡 天 IRAS 12, 25, 60, 100μm 1983ISO 2.5-240μm 1995-19982MASSSIRTF 2.5-200 μm 2003WIRE 12, 25μm 1998The Two Micron All Sky Survey (2MASS) project Two Matching 1.3m Telescopes, Optimized for Efficient Sky Coverage Sites are Mt. Hopkins and CTIO Cameras include 3 infrared arrays, 256 × 256 -- one for each the three bands ( J (1.25 µm), H (1.65 µm), and Ks (2.17 µm) Camera Pixel Size is 2.0“ x 2.0“ Tilting secondary motion during declination scanning freezes frames. 1.3 second exposure time per frame x 6 frames per source = 7.8s integration time. Sub-stepping in both the in-scan and cross-scan direction minimizes effects of undersampling due to large pixels. Mapping Rate of 70 sq. deg./band/night 3C178MHz5C178MHz 6C151 MHz 8C38 MHz Texas365 MHz 87GB4.85 MHz GB64.85 MHz Parkes2.7 MHz NVSS1.4 MHz FIRST1.4 MHz射 电 巡 天 (38MHz-4.85GHz)NVSS(NRAO VLA Sky Survey) NVSS是利用VLA系统在1.4GHz对赤纬-40 (J2000.0)的天区进行射电巡天，角分辨率约为45“ ，5的灵敏度约2.4mJy。

它在1997年底结束，巡天 范围达天球表面积的82%它的主要结果有 (1)2326幅4×4 射电天图，每幅图中有约一千个射电 源，并包含Stokes的I、Q、U三个分量的偏振信息 ； (2)约1,800,000个分离射电源星表，流量密度 S2.5mJy，表中有各源的射电坐标、1.4GHz的射 电流量、偏振流量、偏振位置角及其测量误差等 The FIRST SurveyFaint Images of the Radio Sky at 20cm -- is a project designed to produce the radio equivalent of the Palomar Observatory Sky Survey over 10,000 square degrees of the North and South Galactic Caps. Using the NRAO Very Large Array (VLA) and an automated mapping pipeline, we produce images with 1.8“ pixels, a typical rms of 0.15 mJy, and a resolution of 5“. At the 1 mJy source detection threshold, there are ~90 sources per square degree, ~35% of which have resolved structure on scales from 2-30“. 全波段, 大样本, 巨信息突出创新思想增强课题意识LAMOST的光谱能力与观测模式Ø 107星系—宇宙大尺度结构与星系物理 Ø 107恒星—恒星物理与银河系结构 Ø 106类星体…—多波段天体物理 观测宇宙学的热点哈勃常数和宇宙的年龄 宇宙中的暗物质 宇宙中的元素丰度 宇宙的大尺度结构 宇宙的背景辐射 活动星系核宇宙的背景辐射哈勃常数和宇宙的年龄测定哈勃常数方法星系和星系团 。