Evidence for chemical evolution in the spectra of high redshift galaxies

施勇1980年11月出生。

南京大学 天文与空间科学学院email: yong@教育经历： 1999.9-­‐2003.7 北京大学，地球物理系，天文专业，学士学位。

2003.8-­‐2008.8 亚利桑那大学（美国），天文学，博士学位。

工作经历： 2008.8-­‐2009.8： 亚利桑那大学（美国），博士后。

2009.9-­‐2013.2: 加州理工学院（美国），博士后。

2013.3至今： 南京大学，教授，博导，国家青年千人。

科研基金项目：国家自然科学基金面上项目，11373021，极端贫金属星系：尘埃特性和恒星形成，2014/01-2017/12，80 万元，在研，主持。

中国科学院战略性先导B专项，XDB09000000, 宇宙结构起源B类先导，2014/01-至今，66万，在研，参与（骨干成员）。

中央组织部青年千人项目（第四批）,2013.1-2015.12, 200万，在研、主持。

江苏省基金杰出青年项目，BK20150014, 2015.7-2018.7, 100万，在研、主持。

空间望远镜项目： • P I o n H erschel O T2 y shi 3 (16.1 h rs, p riority 1):“Extremely-­‐metal p oor g alaxies: m apping d ust e mission”• T echnical C ontact a nd C o-­‐I o n S pitzer-­‐50507, 50508 (14.2 h rs, P I: G. R ieke)“Quasar a nd U LIRG E volution”• T echnical C ontact∗ a nd C o-­‐I o n S pitzer-­‐50196 (25.1 h rs, P I: G. R ieke.):“Cosmic Evolution of Star Formation in Quasar Hosts from z=1 to the Present”• T echnical C ontact∗ a nd C o-­‐I o n S pitzer-­‐40385 (2.1 h rs, P I: G. R ieke.):“A C hallenge t o t he U nification M odel”地面望远镜项目：• K eck 10 m: D EIMOS• I RAM 30 m: 24 h rs (2014A), 59.5 h rs (2016A).• P alomar 200 i nch: D BSP; L FC; W IRC• C FHT: M egaCAM• B ok 2.3 m• A rizona R adio O bservatory N RAO-­‐12m• A rizona R adio O bservatory S MT-­‐10m学术服务：ApJ, A pJL, A&A, A J, S ciChina, R AA的审稿人Telescope A ccess P rogram 望远镜分配委员会委员论文发表情况汇总（共36篇）通讯作者 非通讯作者 总计Nature 1 0 1Nature子刊 0 1 117 18 35ApJ, ApJS, ApJL,MNRAS, A&A(全部为NatureIndex高影响力科学期刊)AJ 0 1 1总计 18 20 38第一或通讯作者论文： 18. Zhang, Z.; Shi, Y* et al. 2016, ApJL, 819, 27“Distributions of quasar hosts on the galaxy main-sequence plane”17. Zhou, L.; Shi, Y* et al. 2016, MNRAS, 458, 772“Spatially resolved dust emission of extremely metal poor galaxies”16. S hi, Y.*, W ang, J., Z hang, Z.-­‐Y. e t a l. 2015, A pJL, 804, 11“The Weak Carbon Monoxide Emission in an Extremely Metal-­‐poor Galaxy, Sextans A”15. S hi, Y.*, A rmus, L., H elou, G. e t a l. 2014, N ature, 514, 335–338“Inefficient s tar f ormation i n e xtremely m etal p oor g alaxies”14. Shi, Y.*, Rieke, G., Ogle, P. et al., 2014, ApJS, 214, 23 “Infrared spectra and photometry o f c omplete s amples o f P G a nd 2MASS q uasars”13. Shi, Y.*, Helou, G., Armus, L. 2013, ApJ, 777, 6 “A Joint Model Of X-­‐ray And Infrared B ackgrounds. I I. C ompton-­‐Thick A GN A bundance”12. Shi, Y.*, Helou, G., et al. 2013, ApJ, 764, 28 “A Joint Model of the X-­‐Ray and Infrared E xtragalactic B ackgrounds. I. M odel C onstruc-­‐ t ion a nd F irst R esults”11. Shi, Y.*, Helou, G., et al. 2011, ApJ, 733, 87 “Extended Schmidt Law: Roles Of Existing S tars I n C urrent S tar F ormation”10. Shi, Y.*, Rieke, G. H., et al. 2010, ApJ, 714, 115 “Unobscured Type 2 Active Galactic N uclei”9. Shi, Y.*, Rieke, G. H., et al. 2009, ApJ, 703, 1107 “Cosmic Evolution of Star Formation i n T ype-­‐1 Q uasar H osts S ince z = 1”8. Shi, Y.*, Rieke, G. H., et al. 2009, ApJ, 697, 1764 “Role of Major Mergers In Cosmic S tar F ormation E volution”7. Shi, Y.*, Rieke, G. H. et al. 2008, ApJ, 688, 794 “BH Accretion in Low-­‐Mass Galaxies S ince z∼1”6. Shi, Y.*, Ogle, P., Rieke, G. H. et al. 2007, ApJ, 669, 841 “Aromatic Features in AGN: S tar-­‐Forming I nfrared L uminosity F unction o f A GN H ost G alaxies”5. Shi, Y.*, Rieke, G. H., Hines, D. C. et al. 2007, ApJ, 655, 781 “Thermal and Nonthermal I nfrared E mission f rom M87”4. Shi, Y.*, Rieke, G. H., Hines, D. C. et al. 2006, ApJ, 653, 127 “9.7 um Silicate Features i n A ctive G alactic N uclei: N ew I nsights i nto U nification M odels”3. Shi, Y.*, Rieke, G. H., Papovich, C. et al. 2006, ApJ, 645, 199 “Morphology of Spitzer 24 u m D etected G alaxies i n t he U DF: T he L inks b etween S tar F or-­‐ m ation and G alaxy M orphology”2. Shi, Y.*, Rieke, G. H., Hines, D. C. et al. 2005, ApJ, 629, 88 “Far-­‐Infrared Observations o f R adio Q uasars a nd F R I I R adio G alaxies”1.Shi, Y., & Xu, R. X.* 2003, ApJ, 596, 75 “Can the Age Discrepancies of NeutronStars B e C ircumvented b y a n A ccretion-­‐assisted T orque?”其他作者论文：20. G uo R. e t a l. (Shi Y. 5th a uthor), 2016, A pJ a ccepted, a rXiv:1604.0712219. Chen, Y. et al. (Shi Y. 4th author), 2016, MNRAS accepted, “Boxy Hα EmissionProfiles i n S tar-­‐Forming G alaxies”18. Bian, W. H. et al. (Shi Y. 4th author), 2016, MNRAS, 456, 4081, “Spectral principal component analysis of mid-infrared spectra of a sample of PG QSOs”17. Wang, J. et al. (Shi Y. 4th author), 2016, MNRAS, 455, 3986, “Dense-gas properties in Arp 220 revealed by isotopologue lines”16. Wang, J. et al. (Shi Y. 7th author), 2014, Nature Communication, 5, 5449 “SiO and C H3OH m ega-­‐masers i n N GC 1068”15. Kirkpatrick, A. et al. (Shi Y. 10th author) , 2014, ApJ, 796, 135 “Early Science with the Large Millimeter Telescope: Exploring the Effect of AGN Activity on the Relationships b etween M olecular G as, D ust, a nd S tar F ormation”14. Wang, J. et al. et al. (Shi Y. 4th author) , 2014, ApJ, 796, 57 “Isotopologues o f Dense G as T racers i n N GC 1068”13. Jin, S. et al. (Shi Y. 4th author), 2014, ApJ, 787, 63 “Color-­‐Magnitude Distribution o f F ace-­‐on n earby G alaxies i n S loan D igital S ky S urvey D R7”12. D ale, D. e t a l. (Shi Y. 6th a uthor), 2014, A pJ, 784, 83 “A T wo-­‐parameter M odel for the Infrared/Submillimeter/Radio Spectral Energy Distributions of Galaxies and A ctive G alactic N uclei”11. Wang, J. et al. (Shi Y. 3rd author), 2013, ApJL, 778, 39 “A SiO 2-­‐1 Survey toward G as-­‐rich A ctive G alaxies”10. Magdis, G. E. et al. (Shi Y. 22th author), 2013, A&A, 558, 136 “Mid-­‐ to far infrared p roperties o f s tar-­‐forming g alaxies a nd a ctive g alactic n uclei”9. Kim, Ji Hoon, et al. (Shi Y. 16th author), 2012, ApJ, 760, 120 “The 3.3 m Polycyclic A romatic H ydrocarbon E mission a s a S tar F ormation R ate I ndicator”8. Wang, J., et al. (Shi Y. 3rd author) 2011, MNRAS, 416, 21 “CS (5-­‐4) survey towards n earby i nfrared b right g alaxies”7. T yler, K. D., R ieke, G. H. e t a l. (Shi Y. 9th a uthor) 2011, A pJ, 738, 56 “The N ature of S tar F ormation a t 24 m i n t he G roup E nvironment a t 0.3 < z < 0.55”6. Wu, Y., et al. (Shi Y. 2nd author) 2011, ApJ, 734, 40 “The Mid-­‐infrared Luminosity Function at z < 0.3 from 5MUSES: Understanding the Star Formation/Active G alactic N ucleus B alance f rom a S pectroscopic V iew”5. W u, Y., e t a l. (Shi Y. 5th a uthor) 2010, A pJ, 723, 895 “Infrared L uminosities a nd Aromatic F eatures i n t he 24um F lux L imited S ample o f 5MUSES”4. Mason, R. E., et al. (Shi Y. 3nd author) 2009, ApJ, 693, 136 “The Origin of the Silicate E mission F eatures i n t he S eyfert 2 G alaxy N GC 2110”3. B allantyne, D. R., e t a l. (Shi Y. 2nd a uthor) 2006, A pJ, 653, 1070 “Does t he A GN Unified M odel E volve w ith R edshift? U sing t he X-­‐Ray B ackground t o P re-­‐ d ict t he Mid-­‐Infrared E mission o f A GNs”2. J iang, L. e t a l. (Shi Y. 4th a uthor) 2006, A J, 132, 2127 “Probing t he E volution o f Infrared P roperties o f z ∼6 Q uasars: S pitzer O bservations”1. Wu, Y. et al. (Shi Y. 4th author) 2004, A&A, 426, 503 “A study of high velocity molecular o utflows w ith a n u p-­‐to-­‐date s ample”。

a rXiv:as tr o-ph/13348v121Mar21**TITLE**ASP Conference Series,Vol.**VOLUME**,**PUBLICATION YEAR****EDITORS**The BMW Deep X–ray Cluster Survey Alberto Moretti,Luigi Guzzo,Sergio Campana,Stefano Covino,Davide Lazzati,Marcella Longhetti,Emilio Molinari,Maria Rosa Panzera,Gianpiero Tagliaferri Osservatorio Astronomico di Brera,Via E.Bianchi 46,I-23807Merate,Italy Ian Dell’Antonio Physics Department,Brown University,Box 1843,Providence,RI,USA Abstract.We describe the main features of the BMW survey of serendip-itous X–ray clusters,based on the still unexploited ROSAT–HRI archival observations.The sky coverage,surface density and first deep optical CCD images of the candidates indicate that this sample can represent an excellent complement to the existing PSPC deep cluster surveys and will provide us with a fully independent probe of the evolution of the cluster abundance,in addition to significantly increasing the number of clusters known at z >0.6.1.Introduction In the last few years,X–ray selected samples of clusters of galaxies have become a formidable tool for cosmology.Deep surveys using ROSAT PSPC archival data have been used to study the evolution of the cluster abundance and X–ray luminosity function (XLF)and constrain cosmological parameters (e.g.Borgani et al.1999).The lack of evolution of the XLF observed for L ∼L ∗≃4·1044h 2erg s −1out to z ∼0.8favours low values for ΩM under reasonable assumptionsabout the evolution of the L −T relation.At the same time,the original hint from the EMSS (Gioia et al 1990;Henry et al.1992)of evolution at the very bright end of the XLF seems to be confirmed (Vikhlinin et al.1998,Nichol et al.1999,Rosati et al.2000and references therein).The main statistical limitation of this conclusion rests with the small sky coverage of the ROSAT deep surveys,which clashes with the intrinsic rarity of highly luminous clusters.XMM–Newton and Chandra are already attracting justified attention as the likely source for future samples,but no significant sets of serendipitously selected clusters can be reasonably expected from these observatories for at least another 2years.This presents the window of opportunity for our survey,which uses data from the ROSAT High–Resolution Imager (HRI)archive.With respect to the PSPC,the HRI offers superior angular resolution.Our results indicate that it is actually a surprisingly good source of samples of high-redshift clusters.Our new X–ray selected sample of candidate clusters of galaxies is based on the recently completed BMW survey of serendipitous X–ray sources over 300012Alberto Moretti et al.Figure1.Left:Sky coverage of the BMW survey,as a function ofX–rayflux and extension of the sources.Right:Same,but for a typicalfaint–source core radius∼10arcsec,compared to some previous X–raycluster surveys(see Rosati et al.2000for relevant references).Note thegood compromise between the fairly large area at intermediatefluxes(∼100sq.deg.around∼10−13erg cm−2s−1),and the depth of theBMW sample(1sq.deg.at2.5×10−14erg cm−2s−1).ROSAT HRIfields.The sample includes287candidates,with a significantly large sky coverage in comparison with other recent deep surveys.We are con-ducting a multi-site imaging campaing to fully identify the cluster sample.First results at ESO and TNG are extremely encouraging:with approximately an 80%rate of photometric confirmation in thefirst subsample of35candidates.2.The BMW ProjectThe Brera Multi-scale Wavelet(BMW)project has currently completed the systematic analysis of about3100HRI pointings using a wavelet detection algo-rithm(Lazzati et al.1999).This resulted in a catalog of∼19000serendipitous sources with measuredfluxes and extensions(Campana et al.1999,Panzera et al.2001).A clever selection of the HRI energy channels produced a reduction of the background noise by a factor of∼3,thus greatly improving the ability to detect low–surface–brightness sources as clusters.The BMW general cata-logue is built excludingfields with|b II|≤20◦or pointed on the LMC and SMC. Furthermore to build BMW cluster catalogue we have excluded cluster–targeted HRIfields to avoid the bias produced by the cluster–cluster angular correlation function,for which we have a clear positive detection in thesefields.Cluster candidates were isolated on the basis of their extension,selecting at a high sig-nificance level(corresponding to>5σ)and using only the well–sampled HRI area between3and15armin off-axis.We ended up with a list of287cluster candidates which were visually classified on the DSS2to reject obvious contam-inants(30rejections,mostly nearby galaxies).The BMW project is still under development such that a small assessment in the absolute number is expected.APS Conf.Ser.Style3 3.Survey Sky CoverageAn important parameter characterising a survey of serendipitous sources as the BMW is its sky coverage,i.e.the effective solid angle covered as a function of the limitingflux.Being based on archival pointings,different parts of the sky are observed with different exposure times.Thus,for each value of the X–ray flux f x the sky coverage is given by the total area of all observedfields with limitingflux f lim≤f x.In addition,due to the radial dependence of the point–spread function(PSF)of the ROSAT X–ray telescope,within a singlefield the effectiveflux limit is different for different off–axis angles and extensions of the sources.For this reason,the effective solid angle covered at different flux limits must be carefully estimated considering the instrumental set–up and the detection and characterisation methods adopted(e.g.Rosati1995).We have thereforefirst estimated the sky coverage of the BMW survey for extended objects by assuming aβmodel withβ=2/3,with a set of different core radii. For each core radius we have convolved the analytic profile with the PSF of the instrument at different off-axis angles and we have calculated the corresponding maximum in the wavelet space.Each HRI image has a detection threshold which is calculated in the wavelet space(Lazzati et al.1999)and is only function of the background.Thus for each image we could estimate directly the limiting detectionflux as a function of both the off-axis angle and source extension.In Figure1we compare the BMW cluster sky coverage to some previous X–ray cluster surveys.This relatively quick and straightforward method has some limitations(e.g.it does not tell us how well the wavelet extension is measured), that need to be explored through simulations.To this end,we are currently running an extensive set of simulations following the approach of Vikhlinin et al.(1998),and thefirst outputs for a small sample offields give results which are very close to the semi–analytic calculation,confirming that the sky coverage of Figure1should be a fair representation of our data.4.First Results from Optical Follow–up¿From the287candidates we have further selected a high priority sample of165 objects by excluding the HRIfields with exposure time smaller then10ksec. In spring2000,we started a long–term program of multi–band photometry and spectroscopy of thesefields,which is currently underway using telescopes in both emispheres(mostly the TNG in La Palma and the ESO3.6m telescopes).We have recently(September2000)reached a total of35candidates for which deep optical imaging has been secured in at least two bands.Preliminary analysis of these observations suggests a success rate(i.e.evidence for a galaxy overdensity correlated with the X–ray source)of about80%.The still unidentified20% fraction does not show any obvious pathology and we plan to add deep imaging in K′band,where the contrast of early–type galaxies is maximised,to definitely ascertain their nature.4Alberto Moretti et al.Figure2.Deep g+r+i images(typical exposure times∼5000 sec)with overlaid ROSAT–HRI X–ray contours,for a few examples of identified groups/clusters in the BMW survey.Indicative redshifts for these clusters range from z∼0.2(top left)to∼0.8(bottom right).In each image thefield of view is3x3arcmin.APS Conf.Ser.Style5D image of BMW080459+241(left,6000sec exposurein r+i Gunn bands)with X–ray contours superimposed,and its colour–magnitude diagram(right).A number of galaxies display a similarcolour along an apparent red sequence(filled dots)and their position onthe sky correlates significantly with the X–ray emission(diamonds overleft image).The colour is that expected for an early–type populationat z=0.6.5.DiscussionA hint of the scientific potential of the BMW catalogue can be obtained from the left panel of Figure4where the expected number of clusters as a function of redshift is plotted.These predictions use the computed BMW sky coverage of the high priority sample(165objects)and integrate the local X–ray luminosity function(De Grandi et al.1999)considering or not the evolution suggested by the RDCS,as reported in Rosati(1999).Simple comparison to the total expected numbers from Figure4would seem to imply that the BMW survey sees evolution in the XLF similar to the RDCS results.However,one has to await for the completion of the identification campaign to be able to place serious constraints on evolution.We should remark here the potential advantage of working with HRI data.In the right panel of Figure4we have plotted the apparent diameters of a rich cluster(r c=250kpc)and of a group of galaxies(r c=100kpc)as a function of redshift,together with a measure of the resolution of the ROSAT HRI compared to the PSPC.As one can see,the PSPC is not as suitable as the HRI for distinguishing groups of galaxies from point-like sources beyond redshift0.4. Of course,this simplistic plot depends on several variables,as the underlying cosmology,the source profile and in particular does not take into account the different noise level of the2instruments.Nevertheless,it shows that we should be able to explore the faint end of the XLF,the realm of groups,which could not be studied from PSPC data.In fact,the potentially large number of clusters in the BMW sample,when compared to prediction of evolution or no–evolution models,could also be produced by a steeper local XLF.References6Alberto Moretti et al.Figure4.Left:Expected integral distribution of BMW clusters asa function of redshift,with or without the evolution of the X–ray lumi-nosity function suggested by the RDCS(Rosati et al.1999).Right:Apparent angular diameter of a rich cluster(core radius250kpc)anda group of galaxies(core radius100kpc)as function of redshift,com-pared to the PSF of the two ROSAT instruments at the same off–axisangle(5armin).Borgani,S.,et al.1999,ApJ,517,40.Campana,S.,et al.1999,ApJ,524,423.De Grandi,S.,et al.1999,ApJ,513,L17.Henry,P.et al.1992,ApJ,386,408.Gioia,I.M.,et al.1990,ApJS,72,567.Lazzati,D.,et al.1999,ApJ,524,414.Nichol,R.C.,et al.1999,ApJ,521,L21Panzera,M.R.,et al.2001,in preparation.Rosati,P.1995,PhD thesis(University of Rome).Rosati,P.,et al.1998,ApJ,492,L21.Rosati,P.,et al.2000,in“Large-scale structure in the X–ray Universe”,in press (astro-ph/0001119).Vikhlinin,A.,et al.1998a,ApJ,498,L21.Vikhlinin,A.,et al.1998b,ApJ,502,558.。

Mass really “warps” space and time. Think of space as a two dimensional sheet. A lot of mass in a small area forms a very deep and narrow funnel. The more space is warped, the slower time flows. Deep in the funnel time passes slowly, away from the funnel it passes “normally”.
THE TWILIGHT ZONE
Light has no mass, but it follows the force of gravity!!! WHY? Einstein’s THEORY OF GENERAL RELATIVITY. Ol’ Albert realized that mass places a stress on both time and space. Thus, light is only following the local space time curvature… and this can cause some… strange… effectS …
What would it look like if a Earth mass black hole passed in front of Albert?
The space time around a star is identical to the space time around a black hole, until you get close to the event horizon. WHAT WE SEE WHEN YOU ARE FALLING IN 1. Redshifted (turn red) until redshifted to infinity (you disappear from view) Time slows until it stops when you reach the event horizon WHAT YOU SEE FALLING IN 1. 2. Squeezed and stretched Looking back out to the universe and all time passes by in an instant!

The process of how black holes are formed from the collapse of massive stars or the merging of neutron stars and their physical properties and characteristics.
Black Hole Types
Different types of black holes including stellar mass black holes, supermassive black holes, and intermediate mass black holes and their characteristics and distribution in the universe.
宇宙ppt课件英文
CATALOGUE
目录
IntroductionThe Structure of the UniverseThe Evolution of the UniverseThe Science of the UniverseThe Applications of the UniverseConclusion
The evolution of stars over time, including the life cycle of stars from birth to death and the different stages of stellar evolution.
Planet Formation
Quasar Properties
The properties of quasars including their luminosity, redshift, and spectral energy distribution.