' spatial resolution allow us to study the relationships between [CII] line emission, star formation rate (SFR), and far-infrared (FIR) emission on spatial scales of $\\sim2$ kpc. In the central $\\sim$4 kpc of HZ4, the [CII]\u002FFIR ratio is $\\sim3\\times10^{-3}$ on global scales as well as on spatially-resolved scales of $\\sim$2 kpc, comparable to the ratio observed in local moderate starburst galaxies such as M82 or M83. For the first time in an individual normal galaxy at this redshift, we find evidence for outflowing gas from the central star-forming region in the direction of the minor-axis of the galaxy. The projected velocity of the outflow is $\\sim400$ km s$^{-1}$, and the neutral gas mass outflow rate is $\\sim3-6$ times higher than the SFR in the central region. Finally, we detect a diffuse component of [CII] emission, or \"[CII]-halo\", that extends beyond the star-forming disk and has a size of $\\sim12$ kpc in diameter. Most likely the outflow, which has a velocity approximately half the escape velocity of the system, is in part responsible for fueling the [CII] extended emission. Together with the kinematic analysis of HZ4 (presented in a forthcoming paper), the analysis supports that HZ4 is a typical star-forming disk at $z\\sim5$ with interstellar medium (ISM) conditions similar to present-day galaxies forming stars at a similar level, driving a galactic outflow that may already play a role in its evolution. ","authors":[{"id":"53f4789fdabfaee2a1df62e8","name":"R. Herrera-Camus"},{"id":"53f43242dabfaee43ec04080","name":"N. Förster Schreiber"},{"id":"560c59dc45cedb3397523d9e","name":"R. Genzel"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"53f42e3adabfaedd74d41bb6","name":"A. Bolatto"},{"id":"53f5919edabfaedebef8045b","name":"R. L. Davies"},{"id":"53f36f79dabfae4b349bbf03","name":"D. Fisher"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"5405d41ddabfae450f3d7175","name":"T. Naab"},{"id":"53f47065dabfaee4dc875a62","name":"T. Shimizu"},{"id":"56170fed45cedb3397bb4f1b","name":"K. Tadaki"},{"name":"H. Übler"}],"id":"60015aed91e01163e836a2c2","num_citation":0,"order":3,"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F21\u002F2101\u002F2101.05279.pdf","title":"A kiloparsec view of a typical star-forming galaxy when the Universe was ~1 Gyr old. Part I. Outflow, halo, and interstellar medium properties","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002F2101.05279"],"versions":[{"id":"60015aed91e01163e836a2c2","sid":"2101.05279","src":"arxiv","year":2021}],"year":2021},{"abstract":"Most present-day galaxies with stellar masses ≥1011 solar masses show no ongoing star formation and are dense spheroids. Ten billion years ago, similarly massive galaxies were typically forming stars at rates of hundreds solar masses per year. It is debated how star formation ceased, on which time scales, and how this “quenching” relates to the emergence of dense spheroids. We measured stellar mass and star-formation rate surface density distributions in star-forming galaxies at redshift 2.2 with ~1-kiloparsec resolution. We find that, in the most massive galaxies, star formation is quenched from the inside out, on time scales less than 1 billion years in the inner regions, up to a few billion years in the outer disks. These galaxies sustain high star-formation activity at large radii, while hosting fully grown and already quenched bulges in their cores.","abstract_zh":"","authors":[{"id":"561e7c7145ce1e596492f45d","name":"S. Tacchella"},{"id":"5434fde9dabfaebba588a80f","name":"C. M. Carollo"},{"id":"53f457cbdabfaedf43610faf","name":"A. Renzini"},{"id":"53f4385edabfaec09f18f8ee","name":"N. M. Förster Schreiber"},{"id":"561e7c7245ce1e596492f466","name":"P. Lang"},{"id":"561e7c7245ce1e596492f469","name":"S. Wuyts"},{"id":"53f44d53dabfaefedbb2ed70","name":"G. Cresci"},{"id":"561e7c7245ce1e596492f46e","name":"A. Dekel"},{"id":"561e7c7245ce1e596492f471","name":"R. Genzel"},{"id":"53f4424bdabfaee0d9ba5196","name":"S. J. Lilly"},{"id":"5409693fdabfae450f481c2e","name":"C. Mancini"},{"id":"53f43753dabfaeb1a7bfc29f","name":"S. Newman"},{"id":"53f42c00dabfaeb22f3f338f","name":"M. Onodera"},{"id":"53f42c79dabfaec09f1072a1","name":"A. Shapley"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"561e7c7345ce1e596492f480","name":"J. Woo"},{"id":"53f43012dabfaee1c0a55d15","name":"G. Zamorani"}],"doi":"10.1126\u002Fscience.1261094","id":"55aa4fa765ce2a9b9e15fc83","lang":"en","num_citation":106,"order":14,"pages":{"end":"317","start":"314"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F15\u002F1504\u002F1504.04021.pdf","title":"Evidence for mature bulges and an inside-out quenching phase 3 billion years after the Big Bang","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1126\u002Fscience.1261094","http:\u002F\u002Fwww.sciencemag.org\u002Fcontent\u002F348\u002F6232\u002F314.abstract","https:\u002F\u002Farxiv.org\u002Fabs\u002F1504.04021"],"venue":{"info":{"name":"science","name_zh":""},"issue":"6232","volume":"348"},"versions":[{"id":"55aa4fa765ce2a9b9e15fc83","sid":"348\u002F6232\u002F314","src":"science","year":2015},{"id":"56d8d8e4dabfae2eeedf76a3","sid":"2158012372","src":"mag","year":2015},{"id":"5c610912da56297340b61026","sid":"1504.04021","src":"arxiv","year":2015}],"year":2015},{"abstract":"The structure of a sample of high-redshift (z similar to 2), rotating galaxies with high star formation rates and turbulent gas velocities of sigma approximate to 40-80 km s(-1) is investigated. Fitting the observed disk rotational velocities and radii with a Mo et al. (MMW) model requires unusually large disk spin parameters lambda(d) \u003E 0.1 and disk-to-dark halo mass fractions of m(d) approximate to 0.2, close to the cosmic baryon fraction. The galaxies segregate into dispersion-dominated systems with 1 \u003C= v(max)\u002Fsigma \u003C= 3, maximum rotational velocities v(max) \u003C= 200 km s(-1), and disk half-light radii r(1\u002F2) approximate to 1-3 kpc, and rotation-dominated systems with v(max) \u003E 200 km s(-1), v(max)\u002Fsigma \u003E 3, and r(1\u002F2) approximate to 4-8 kpc. For the dispersion-dominated sample, radial pressure gradients partly compensate the gravitational force, reducing the rotational velocities. Including this pressure effect in the MMW model, dispersion-dominated galaxies can be fitted well with spin parameters of lambda(d) = 0.03-0.05 for high disk mass fractions of m(d) approximate to 0.2 and with lambda(d) = 0.01-0.03 for m(d) approximate to 0.05. These values are in good agreement with cosmological expectations. For the rotation-dominated sample, however, pressure effects are small and better agreement with theoretically expected disk spin parameters can only be achieved if the dark halo mass contribution in the visible disk regime (2-3 x r(1\u002F2)) is smaller than predicted by the MMW model. We argue that these galaxies can still be embedded in standard cold dark matter halos if the halos do not contract adiabatically in response to disk formation. In this case, the data favor models with small disk mass fractions of m(d) = 0.05 and disk spin parameters of lambda(d) approximate to 0.035. It is shown that the observed high turbulent gas motions of the galaxies are consistent with a Toomre instability parameter Q = 1 which is equal to the critical value, expected for gravitational disk instability to be the major driver of turbulence. The dominant energy source of turbulence is then the potential energy of the gas in the disk.","abstract_zh":"","authors":[{"id":"54410e44dabfae7d84bdbb7a","name":"A. Burkert"},{"id":"5609f6e445cedb3396fed237","name":"R. Genzel"},{"id":"53f44438dabfaedf435c40b2","name":"N. Bouche"},{"id":"53f44d53dabfaefedbb2ed70","name":"G. Cresci"},{"id":"53f39691dabfae4b34a76080","name":"S. Khochfar"},{"id":"53f4395bdabfaedce554b04a","name":"J. Sommer-Larsen"},{"id":"53f586dedabfaeb1d1f8045c","name":"A. Sternberg"},{"id":"53f47718dabfaedf43687c1f","name":"T. Naab"},{"id":"53f43242dabfaee43ec04080","name":"N. Foerster-Schreiber"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"5440d55bdabfae7d84bbca03","name":"K. Shapiro"},{"id":"53f42e27dabfaee1c0a3dad7","name":"E. Hicks"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"name":"R. Davies"},{"id":"53f45646dabfaedd74e2d87b","name":"P. Buschkamp"},{"id":"53f4332adabfaeb22f450a6c","name":"S. Genel"}],"doi":"10.1088\u002F0004-637X\u002F725\u002F2\u002F2324","id":"53e9b63ab7602d9704194fcd","lang":"en","num_citation":79,"order":9,"pages":{"end":"2332","start":"2324"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F09\u002F0907\u002F0907.4777.pdf","title":"High-Redshift Star-Forming Galaxies: Angular Momentum and Baryon Fraction, Turbulent Pressure Effects and the Origin of Turbulence","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1088\u002F0004-637X\u002F725\u002F2\u002F2324","https:\u002F\u002Farxiv.org\u002Fabs\u002F0907.4777","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"725"},"versions":[{"id":"53e27fc320f7fff6783044ce","sid":"27627365","src":"msra","year":2009},{"id":"56d837a1dabfae2eee4af953","sid":"1978007991","src":"mag","year":2009},{"id":"5c6106d8da56297340adf1b1","sid":"0907.4777","src":"arxiv","year":2010},{"id":"5fc6f967d75e2ac63d5940d4","sid":"WOS:000285501300077","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2010}],"year":2010},{"abstract":"We present the modeling of SINFONI integral field dynamics of 18 star-forming galaxies at z similar to 2 from Ha line emission. The galaxies are selected from the larger sample of the SINS survey, based on the prominence of ordered rotational motions with respect to more complex merger-induced dynamics. The quality of the data allows us to carefully select systems with kinematics dominated by rotation, and to model the gas dynamics across the whole galaxy using suitable exponential disk models. We obtain a good correlation between the dynamical mass and the stellar mass, finding that large gas fractions (M-gas approximate to M*) are required to explain the are required to explain the difference between the two quantities. We use the derived stellar mass and maximum rotational velocity V-max from the modeling to construct for the first time the stellar mass Tully-Fisher relation at z similar to 2.2. The relation obtained shows a slope similar to what is observed at lower redshift, but we detect an evolution of the zero point. We find that at z similar to 2.2 there is an offset in log(M*) for a given rotational velocity of 0.41 +\u002F- 0.11 with respect to the local universe. This result is consistent with the predictions of the latest N-body\u002Fhydrodynamical simulations of disk formation and evolution, which invoke gas accretion onto the forming disk in filaments and cooling flows. This scenario is in agreement with other dynamical evidence from SINS, where gas accretion from the halo is required to reproduce the observed properties of a large fraction of the z similar to 2 galaxies.","authors":[{"id":"53f44d53dabfaefedbb2ed70","name":"G. Cresci"},{"id":"53f42e27dabfaee1c0a3dad7","name":"E. K. S. Hicks"},{"id":"560406f045cedb33962d14cf","name":"R. Genzel"},{"id":"53f4385edabfaec09f18f8ee","name":"N. M. Förster Schreiber"},{"id":"53f5919edabfaedebef8045b","name":"R. Davies"},{"id":"53f46d13dabfaee1c0b81b3f","name":"N. Bouché"},{"id":"53f45646dabfaedd74e2d87b","name":"P. Buschkamp"},{"id":"53f4332adabfaeb22f450a6c","name":"S. Genel"},{"id":"5440d55bdabfae7d84bbca03","name":"K. Shapiro"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"53f4395bdabfaedce554b04a","name":"J. Sommer-Larsen"},{"id":"54410e44dabfae7d84bdbb76","name":"A. Burkert"},{"id":"5440ff8cdabfae805a7197f7","name":"F. Eisenhauer"},{"id":"53f4652adabfaee02ad8f795","name":"O. Gerhard"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"53f47718dabfaedf43687c1f","name":"T. Naab"},{"id":"53f586dedabfaeb1d1f8045c","name":"A. Sternberg"},{"id":"548811b1dabfae8a11fb406c","name":"A. Cimatti"},{"id":"53f44dfbdabfaee02ad379e0","name":"E. Daddi"},{"id":"53f45e11dabfaee02ad74852","name":"D. K. Erb"}],"doi":"10.1088\u002F0004-637X\u002F697\u002F1\u002F115","id":"53e99fd0b7602d97028af082","lang":"en","num_citation":0,"order":9,"pages":{"end":"132","start":"115"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F09\u002F0902\u002F0902.4701.pdf","title":"THE SINS SURVEY: MODELING THE DYNAMICS OF\u003Ci\u003Ez\u003C\u002Fi\u003E∼ 2 GALAXIES AND THE HIGH-\u003Ci\u003Ez\u003C\u002Fi\u003ETULLY-FISHER RELATION","venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"1","volume":"697"},"versions":[{"id":"53e2b5ed20f7fff6791a5f47","sid":"43158312","src":"msra","year":2009},{"id":"5c610689da56297340ac6a8a","sid":"0902.4701","src":"arxiv","year":2009},{"id":"5fc6f98dd75e2ac63d595273","sid":"WOS:000265764000012","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2009}],"year":2009},{"abstract":"We present initial results from a survey of nearby AGN using the near infrared adaptive optics integral field spectrograph SINFONI. These data enable us to probe the distribution and kinematics of the gas and stars at spatial resolutions as small as 0.085 \", corresponding in some cases to less than 10 pc. In this contribution we present results concerning (1) the molecular gas in the nucleus of NGC 1068 and its relation to the obscuring torus; and (2) the stars which exist on spatial scales of a few tens of parsecs around the AGN, the evidence for their remarkably young age and extreme intensities, and their relation to the AGN.","abstract_zh":"","authors":[{"id":"5603d07b45cedb339625aa08","name":"Richard Davies"},{"id":"5440aa01dabfae7d84b9e0e2","name":"Reinhard Genzel"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"53f44d1bdabfaec09f1e3510","name":"F. Mueller Sánchez"},{"id":"53f586dedabfaeb1d1f8045c","name":"A. Sternberg"}],"doi":"10.1007\u002F978-0-387-72768-4_21","id":"53e99f03b7602d97027d243e","lang":"en","num_citation":0,"order":2,"pages":{"end":"+","start":"144"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F06\u002F0610\u002Fastro-ph0610203.pdf","title":"Star Formation and Molecular Gas in AGN","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1007\u002F978-0-387-72768-4_21","https:\u002F\u002Farxiv.org\u002Fabs\u002Fastro-ph\u002F0610203","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"Astrophysics and Space Science Proceedings"},"issue":"","volume":""},"versions":[{"id":"53e2805a20f7fff678326799","sid":"27767344","src":"msra","year":0},{"id":"56d84246dabfae2eee92153c","sid":"1657487024","src":"mag","year":2006},{"id":"5c75076ff56def9798597b37","sid":"1657487024","src":"mag","vsid":"2595170531","year":2008},{"id":"5c6109eada56297340b98408","sid":"astro-ph\u002F0610203","src":"arxiv","year":2006},{"id":"5ff1d0bf19519e9c39698f19","sid":"WOS:000250578600021","src":"wos","vsid":"Astrophysics and Space Science Proceedings","year":2008}],"year":2008},{"abstract":"We present a detailed analysis of the spatially resolved properties of the lensed submillimeter galaxy (SMG) SMM J14011+0252 at z = 2.56, combining deep near-infrared integral-field data obtained with SPIFFI on the VLT with other multiwavelength data sets. As previously discussed by other authors, the broad characteristics of SMMJ14011+0252 in particular and submillimeter galaxies in general are in agreement with what is expected for the early evolution of local massive spheroidal galaxies. From continuum and line flux, velocity, and dispersion maps, we measure the kinematics, star formation rates, gas densities, and extinction for individual subcomponents. The star formation intensity is similar to low-redshift \"maximal starbursts,\" while the line fluxes and the dynamics of the emission line gas provide direct evidence for a starburst-driven wind with physical properties very similar to local superwinds. We also find circumstantial evidence for \"self-regulated\" star formation within J1. The relative velocity of the bluer companion J2 yields a dynamical mass estimate for J1 within similar to 20 kpc of M-dyn similar to 1 x 10(11) M.. The relative metallicity of J2 is 0.4 dex lower than in J1n\u002FJ1s, suggesting different star formation histories. Spectral energy distribution fitting of the continuum peak J1c confirms and substantiates previous suggestions that this component is a z = 0.25 interloper. When removing J1c, the stellar continuum and H alpha line emission appear well aligned spatially in two individual components, J1n and J1s, and coincide with two kinematically distinct regions in the velocity map, which might well indicate a merging system. This highlights the close similarity between SMGs and ultraluminous infrared galaxies (ULIRGs), which are often merger-driven maximal starbursts, and suggests that the intrinsic mechanisms of star formation and related feedback are in fact similar to low-redshift strongly star-forming systems.","authors":[{"id":"53f470d7dabfaeee22a7a435","name":"N. P. H. Nesvadba"},{"id":"560923ae45cedb3396e2f74d","name":"M. D. Lehnert"},{"id":"560923ae45cedb3396e2f750","name":"R. Genzel"},{"id":"5440ff8cdabfae805a7197f7","name":"F. Eisenhauer"},{"id":"53f42f96dabfaee43ebe1570","name":"A. J. Baker"},{"id":"53f44b49dabfaee02ad2cda0","name":"S. Seitz"},{"id":"53f5919edabfaedebef8045b","name":"R. Davies"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"53f46714dabfaedd74e6c7a0","name":"M. Tecza"},{"id":"53f42f13dabfaec22ba2d81d","name":"R. Bender"},{"id":"53f42ee9dabfaee0d9b109c2","name":"R. Abuter"}],"doi":"10.1086\u002F511151","id":"53e9b355b7602d9703e3201d","lang":"en","num_citation":7,"order":8,"pages":{"end":"737","start":"725"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F06\u002F0611\u002Fastro-ph0611769.pdf","title":"Intense Star Formation and Feedback at High Redshift: Spatially Resolved Properties of the\u003Ci\u003Ez\u003C\u002Fi\u003E= 2.6 Submillimeter Galaxy SMM J14011+0252","venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"657"},"versions":[{"id":"53e2b5ed20f7fff6791a54ea","sid":"43155659","src":"msra","year":2007},{"id":"5c6109ecda56297340b98b2c","sid":"astro-ph\u002F0611769","src":"arxiv","year":2006},{"id":"5fc6f9bcd75e2ac63d596a6c","sid":"WOS:000244928500007","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2007}],"year":2007},{"abstract":"We present some preliminary (half-way) results on our adaptive optics spectroscopic survey of AGN at spatial scales down to 0.085 \". Most of the data were obtained with SINFONI which provides integral field capability at a spectral resolution of R similar to 4000. The themes on which we focus in this contribution are: star formation around the AGN, the properties of the molecular gas and its relation to the torus, and the mass of the black bole.","abstract_zh":"","authors":[{"id":"53f5919edabfaedebef8045b","name":"R. Davies"},{"id":"5605104745cedb33965411be","name":"R. Genzel"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"53f318ccdabfae9a84427df5","name":"F. Müller Sanchez"},{"id":"53f56084dabfae5aacf80461","name":"j. Thomas"},{"id":"544838dcdabfae87b7debf4f","name":"S. Friedrich"}],"doi":"10.1007\u002F978-3-540-73491-8_41","id":"53e9a41db7602d9702d39985","lang":"en","num_citation":0,"order":2,"pages":{"end":"263","start":"259"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F06\u002F0601\u002Fastro-ph0601417.pdf","title":"SINFONI’s take on Star Formation, Molecular Gas, and Black Hole Masses in AGN","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1007\u002F978-3-540-73491-8_41","https:\u002F\u002Farxiv.org\u002Fabs\u002Fastro-ph\u002F0601417","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ESO ASTROPHYSICS SYMPOSIA"},"issue":"","volume":""},"versions":[{"id":"53e2805a20f7fff678326960","sid":"27767799","src":"msra","year":0},{"id":"56d855cedabfae2eee273f2d","sid":"1521495092","src":"mag","year":2006},{"id":"5c7501e4f56def97984b4746","sid":"1521495092","src":"mag","vsid":"2595170531","year":2007},{"id":"5c6109e3da56297340b968e0","sid":"astro-ph\u002F0601417","src":"arxiv","year":2006},{"id":"5fc77ebf5016bf8811fcbb78","sid":"WOS:000251479500041","src":"wos","vsid":"ESO ASTROPHYSICS SYMPOSIA","year":2007}],"year":2007},{"abstract":"We present a detailed analysis of the spatially resolved properties of the lensed submillimeter galaxy (SMG) SMM J14011+0252 at z = 2.56, combining deep near-infrared integral-field data obtained with SPIFFI on the VLT with other multiwavelength data sets. As previously discussed by other authors, the broad characteristics of SMMJ14011+0252 in particular and submillimeter galaxies in general are in agreement with what is expected for the early evolution of local massive spheroidal galaxies. From continuum and line flux, velocity, and dispersion maps, we measure the kinematics, star formation rates, gas densities, and extinction for individual subcomponents. The star formation intensity is similar to low-redshift \"maximal starbursts,\" while the line fluxes and the dynamics of the emission line gas provide direct evidence for a starburst-driven wind with physical properties very similar to local superwinds. We also find circumstantial evidence for \"self-regulated\" star formation within J1. The relative velocity of the bluer companion J2 yields a dynamical mass estimate for J1 within similar to 20 kpc of M-dyn similar to 1 x 10(11) M.. The relative metallicity of J2 is 0.4 dex lower than in J1n\u002FJ1s, suggesting different star formation histories. Spectral energy distribution fitting of the continuum peak J1c confirms and substantiates previous suggestions that this component is a z = 0.25 interloper. When removing J1c, the stellar continuum and H alpha line emission appear well aligned spatially in two individual components, J1n and J1s, and coincide with two kinematically distinct regions in the velocity map, which might well indicate a merging system. This highlights the close similarity between SMGs and ultraluminous infrared galaxies (ULIRGs), which are often merger-driven maximal starbursts, and suggests that the intrinsic mechanisms of star formation and related feedback are in fact similar to low-redshift strongly star-forming systems.","abstract_zh":"","authors":[{"id":"53f470d7dabfaeee22a7a435","name":"N. P. H. Nesvadba"},{"id":"560b638745cedb33972f633a","name":"M. D. Lehnert"},{"id":"560b638745cedb33972f633d","name":"R. Genzel"},{"id":"5440ff8cdabfae805a7197f7","name":"F. Eisenhauer"},{"id":"53f42f96dabfaee43ebe1570","name":"A. J. Baker"},{"name":"S. Seitz"},{"id":"53f5919edabfaedebef8045b","name":"R. Davies"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"53f46714dabfaedd74e6c7a0","name":"M. Tecza"},{"id":"53f42f13dabfaec22ba2d81d","name":"R. Bender"},{"id":"53f42ee9dabfaee0d9b109c2","name":"R. Abuter"}],"doi":"10.1086\u002F511151","id":"53e9baf2b7602d970472316c","lang":"en","num_citation":38,"order":8,"pages":{"end":"737","start":"725"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F06\u002F0611\u002Fastro-ph0611769.pdf","title":"Intense Star-formation and Feedback at High Redshift: Spatially-resolved Properties of the z=2.6 Submillimeter Galaxy SMMJ14011+0252","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1086\u002F511151","https:\u002F\u002Farxiv.org\u002Fabs\u002Fastro-ph\u002F0611769","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"657"},"versions":[{"id":"53e2645220f7fff6779b1d3d","sid":"12820147","src":"msra","year":2006},{"id":"56d8378ddabfae2eee4a6f4f","sid":"1964216776","src":"mag","year":2006},{"id":"5c6109ecda56297340b98b2c","sid":"astro-ph\u002F0611769","src":"arxiv","year":2006},{"id":"5fc6f9bcd75e2ac63d596a6c","sid":"WOS:000244928500007","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2007}],"year":2007},{"abstract":"Using the near-infrared integral field spectrograph SPIFFI on the VLT, we have studied the spatially resolved dynamics in the z = 3.2 strongly lensed galaxy 1E 0657-56 arc+core by observing the rest-frame optical emission lines [OIII] lambda 5007 and H beta. The lensing configuration suggests that the high surface brightness core is the M similar to 20 magnified central similar to 1 kpc of the galaxy, whereas the fainter arc is the more strongly magnified peripheral region of the same galaxy at about a half-light radius, which otherwise appears to be a typical z similar to 3 Lyman break galaxy. The overall shape of the position-velocity diagram resembles the rotation curves of the inner few kpc of nearby similar to L* spiral galaxies. For M = 20, our data have a spatial resolution of similar to 200 pc in the source plane. The projected velocities v rot rise rapidly to similar to 75 km s(-1) within radii similar to 0.5 kpc from the center and asymptotically reach a velocity of similar to 190 km s(-1) within the arc, at a projected radius of a few kpc radius. The rotation curve implies a dynamical mass of log M-dyn\u002FM similar to 9.3 within the central kpc and suggests that in this system the equivalent of the mass of a present-day similar to L* bulge at the same radius was already in place by z \u003E= 3. Approximating the circular velocity of the halo by the measured asymptotic velocity of the rotation curve, we estimate a dark matter halo mass of log M-halo\u002FM similar to 11.7 +\u002F- 0.3, in good agreement with large-scale clustering studies of Lyman break galaxies. The baryonic collapse fraction is low compared to z similar to 2 actively star-forming BX and low-redshift galaxies, perhaps implying comparatively less gas infall to small radii or efficient feedback. Even more speculatively, the high central mass density might indicate highly dissipative gas collapse in very early stages of galaxy evolution, in approximate agreement with what is expected for \"inside-out\" galaxy formation models.","abstract_zh":"","authors":[{"id":"53f470d7dabfaeee22a7a435","name":"N. P. H. Nesvadba"},{"id":"5607bc3445cedb3396b4efee","name":"M. D. Lehnert"},{"id":"5440ff8cdabfae805a7197f7","name":"F. Eisenhauer"},{"id":"5607bc3445cedb3396b4eff1","name":"R. Genzel"},{"name":"S. Seitz"},{"id":"5607bc3445cedb3396b4eff4","name":"R. I. Davies"},{"id":"54329761dabfaeb4c6a90d3f","name":"R. P. Saglia"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"53f42f13dabfaec22ba2d81d","name":"R. Bender"},{"id":"53f42ee9dabfaee0d9b109c2","name":"R. Abuter"}],"doi":"10.1086\u002F507090","id":"53e9aea4b7602d97038c66fc","lang":"en","num_citation":10,"order":8,"pages":{"end":"668","start":"661"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F06\u002F0606\u002Fastro-ph0606527.pdf","title":"Lyman Break Galaxies Under a Microscope: The Small Scale Dynamics and Mass of an Arc in the Cluster 1E0657-56","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1086\u002F507090","https:\u002F\u002Farxiv.org\u002Fabs\u002Fastro-ph\u002F0606527","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"650"},"versions":[{"id":"53e262e320f7fff67796ae8c","sid":"12454361","src":"msra","year":2006},{"id":"56d837a1dabfae2eee4afcd3","sid":"2055789659","src":"mag","year":2006},{"id":"5c6109e7da56297340b97878","sid":"astro-ph\u002F0606527","src":"arxiv","year":2006},{"id":"5fc6f899d75e2ac63d58e063","sid":"WOS:000241497700011","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2006}],"year":2006},{"abstract":"Using the near-infrared integral field spectrograph SPIFFI on the VLT, we have studied the spatially resolved dynamics in the z = 3.2 strongly lensed galaxy 1E 0657-56 arc+core by observing the rest-frame optical emission lines [OIII] lambda 5007 and H beta. The lensing configuration suggests that the high surface brightness core is the M similar to 20 magnified central similar to 1 kpc of the galaxy, whereas the fainter arc is the more strongly magnified peripheral region of the same galaxy at about a half-light radius, which otherwise appears to be a typical z similar to 3 Lyman break galaxy. The overall shape of the position-velocity diagram resembles the rotation curves of the inner few kpc of nearby similar to L* spiral galaxies. For M = 20, our data have a spatial resolution of similar to 200 pc in the source plane. The projected velocities v rot rise rapidly to similar to 75 km s(-1) within radii similar to 0.5 kpc from the center and asymptotically reach a velocity of similar to 190 km s(-1) within the arc, at a projected radius of a few kpc radius. The rotation curve implies a dynamical mass of log M-dyn\u002FM similar to 9.3 within the central kpc and suggests that in this system the equivalent of the mass of a present-day similar to L* bulge at the same radius was already in place by z \u003E= 3. Approximating the circular velocity of the halo by the measured asymptotic velocity of the rotation curve, we estimate a dark matter halo mass of log M-halo\u002FM similar to 11.7 +\u002F- 0.3, in good agreement with large-scale clustering studies of Lyman break galaxies. The baryonic collapse fraction is low compared to z similar to 2 actively star-forming BX and low-redshift galaxies, perhaps implying comparatively less gas infall to small radii or efficient feedback. Even more speculatively, the high central mass density might indicate highly dissipative gas collapse in very early stages of galaxy evolution, in approximate agreement with what is expected for \"inside-out\" galaxy formation models.","authors":[{"id":"53f470d7dabfaeee22a7a435","name":"N. P. H. Nesvadba"},{"id":"5607bc3445cedb3396b4eff7","name":"M. D. Lehnert"},{"id":"5440ff8cdabfae805a7197f7","name":"F. Eisenhauer"},{"id":"5607bc3545cedb3396b4effa","name":"R. Genzel"},{"id":"53f44b49dabfaee02ad2cda0","name":"S. Seitz"},{"id":"5607bc3545cedb3396b4effd","name":"R. I. Davies"},{"id":"54329761dabfaeb4c6a90d3f","name":"R. P. Saglia"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"53f42f13dabfaec22ba2d81d","name":"R. Bender"},{"id":"53f42ee9dabfaee0d9b109c2","name":"R. Abuter"}],"doi":"10.1086\u002F507090","id":"53e9aea4b7602d97038c6704","lang":"en","num_citation":29,"order":8,"pages":{"end":"668","start":"661"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F06\u002F0606\u002Fastro-ph0606527.pdf","title":"Lyman Break Galaxies under a Microscope: The Small‐Scale Dynamics and Mass of an Arc in the Cluster 1E 0657−56","venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"650"},"versions":[{"id":"53e2b5ed20f7fff6791a5311","sid":"43155186","src":"msra","year":2006},{"id":"5c6109e7da56297340b97878","sid":"astro-ph\u002F0606527","src":"arxiv","year":2006},{"id":"5fc6f899d75e2ac63d58e063","sid":"WOS:000241497700011","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2006}],"year":2006},{"abstract":"We discuss identifications for 18 sources from our Max-Planck-Millimeter-Bolometer ( MAMBO) 1.2 mm survey of the region surrounding the NTT Deep Field. We have obtained accurate positions from Very Large Array 1.4 GHz interferometry, and in a few cases IRAM millimeter interferometry, and have also made deep BVRIzJK imaging at ESO. We find thirteen 1.2 mm sources associated with optical\u002Fnear-infrared objects in the magnitude range K = 19.0-22.5, while five are blank fields at K \u003E 22. We argue from a comparison of optical\u002Fnear-infrared photometric redshifts and radio\u002Fmillimeter redshift estimates that two of the 13 optical\u002Fnear-infrared objects are likely foreground objects distinct from the dust sources, one of them possibly lensing the millimeter source. The median redshift of the radio-identified millimeter sources is similar to2.6 from the radio\u002Fmillimeter estimator, and the median optical\u002Fnear-infrared photometric redshifts for the objects with counterparts is similar to2.1. This suggests that those radio-identified millimeter sources without optical\u002Fnear-infrared counterparts tend to lie at higher redshifts than those with optical\u002Fnear-infrared counterparts. Compared to published identifications of objects from 850 mum surveys of similar depth, the median K and I magnitudes of our counterparts are roughly 2 mag fainter, and the dispersion of I-K colors is less. Real differences in the median redshifts, residual misidentifications with bright objects, cosmic variance, and small-number statistics are likely to contribute to this significant difference, which also affects redshift measurement strategies. Some of the counterparts are red in J-K (greater than or similar to20%), but the contribution of such millimeter objects to the recently studied population of near-infrared selected (J(s)-K-s \u003E 2.3) high-redshift galaxies is only of order a few percent. The recovery rate of MAMBO sources by preselection of optically faint radio sources is relatively low (similar to25%), in contrast to some claims of a higher rate for Submillimeter Common-User Bolometric Array ( SCUBA) sources (similar to70%). In addition to this difference, the MAMBO sources also appear significantly fainter (similar to1.5 mag in the I band) than radio-preselected SCUBA sources. We discuss the basic properties of the near-infrared\u002F(sub)millimeter\u002Fradio spectral energy distributions of our galaxies and of interferometrically identified submillimeter sources from the literature. From a comparison with submillimeter objects with CO-confirmed spectroscopic redshifts, we argue that roughly two-thirds of the ( sub) millimeter galaxies are at z greater than or similar to 2.5. This fraction is probably larger when including sources without radio counterparts.","authors":[{"id":"53f4460bdabfaedd74decc15","name":"H. Dannerbauer"},{"id":"5604963f45cedb3396425c53","name":"M. D. Lehnert"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"544820d1dabfae87b7ddcaef","name":"F. Bertoldi"},{"id":"53f47371dabfaedd74e9d2e6","name":"C. Carilli"},{"id":"5604963f45cedb3396425c56","name":"R. Genzel"},{"id":"53f4ce73dabfaeed1ff819bc","name":"K. M. Menten"}],"doi":"10.1086\u002F383138","id":"53e9a224b7602d9702b27487","lang":"en","num_citation":0,"order":3,"pages":{"end":"682","start":"664"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F04\u002F0402\u002Fastro-ph0402549.pdf","title":"The faint counterparts of MAMBO mm sources near the NTT Deep Field","venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"606"},"versions":[{"id":"53e2637720f7fff67799155d","sid":"12633188","src":"msra","year":2004},{"id":"5c6109d2da56297340b92220","sid":"astro-ph\u002F0402549","src":"arxiv","year":2004},{"id":"5fc6f9f7d75e2ac63d598bf5","sid":"WOS:000221261900005","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2004}],"year":2004},{"abstract":"We discuss identifications for 18 sources from our Max-Planck-Millimeter-Bolometer ( MAMBO) 1.2 mm survey of the region surrounding the NTT Deep Field. We have obtained accurate positions from Very Large Array 1.4 GHz interferometry, and in a few cases IRAM millimeter interferometry, and have also made deep BVRIzJK imaging at ESO. We find thirteen 1.2 mm sources associated with optical\u002Fnear-infrared objects in the magnitude range K = 19.0-22.5, while five are blank fields at K \u003E 22. We argue from a comparison of optical\u002Fnear-infrared photometric redshifts and radio\u002Fmillimeter redshift estimates that two of the 13 optical\u002Fnear-infrared objects are likely foreground objects distinct from the dust sources, one of them possibly lensing the millimeter source. The median redshift of the radio-identified millimeter sources is similar to2.6 from the radio\u002Fmillimeter estimator, and the median optical\u002Fnear-infrared photometric redshifts for the objects with counterparts is similar to2.1. This suggests that those radio-identified millimeter sources without optical\u002Fnear-infrared counterparts tend to lie at higher redshifts than those with optical\u002Fnear-infrared counterparts. Compared to published identifications of objects from 850 mum surveys of similar depth, the median K and I magnitudes of our counterparts are roughly 2 mag fainter, and the dispersion of I-K colors is less. Real differences in the median redshifts, residual misidentifications with bright objects, cosmic variance, and small-number statistics are likely to contribute to this significant difference, which also affects redshift measurement strategies. Some of the counterparts are red in J-K (greater than or similar to20%), but the contribution of such millimeter objects to the recently studied population of near-infrared selected (J(s)-K-s \u003E 2.3) high-redshift galaxies is only of order a few percent. The recovery rate of MAMBO sources by preselection of optically faint radio sources is relatively low (similar to25%), in contrast to some claims of a higher rate for Submillimeter Common-User Bolometric Array ( SCUBA) sources (similar to70%). In addition to this difference, the MAMBO sources also appear significantly fainter (similar to1.5 mag in the I band) than radio-preselected SCUBA sources. We discuss the basic properties of the near-infrared\u002F(sub)millimeter\u002Fradio spectral energy distributions of our galaxies and of interferometrically identified submillimeter sources from the literature. From a comparison with submillimeter objects with CO-confirmed spectroscopic redshifts, we argue that roughly two-thirds of the ( sub) millimeter galaxies are at z greater than or similar to 2.5. This fraction is probably larger when including sources without radio counterparts.","abstract_zh":"","authors":[{"id":"53f4460bdabfaedd74decc15","name":"H. Dannerbauer"},{"id":"5604459545cedb3396362dc6","name":"M. D. Lehnert"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"544820d1dabfae87b7ddcaef","name":"F. Bertoldi"},{"name":"C. Carilli"},{"id":"5604459545cedb3396362dc9","name":"R. Genzel"},{"id":"53f4ce73dabfaeed1ff819bc","name":"K. M. Menten"}],"doi":"10.1086\u002F383138","id":"53e9a0d2b7602d97029bcf44","lang":"en","num_citation":68,"order":3,"pages":{"end":"682","start":"664"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F04\u002F0402\u002Fastro-ph0402549.pdf","title":"The Faint Counterparts of MAMBO Millimeter Sources near the New Technology Telescope Deep Field","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1086\u002F383138","https:\u002F\u002Farxiv.org\u002Fabs\u002Fastro-ph\u002F0402549","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"606"},"versions":[{"id":"53e2b5e620f7fff6791a476c","sid":"43152205","src":"msra","year":2004},{"id":"56d837a4dabfae2eee4b0d96","sid":"2059696663","src":"mag","year":2004},{"id":"5c6109d2da56297340b92220","sid":"astro-ph\u002F0402549","src":"arxiv","year":2004},{"id":"5fc6f9f7d75e2ac63d598bf5","sid":"WOS:000221261900005","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2004}],"year":2004},{"abstract":"We describe the first results of a programme to obtain rotation curves of z~1\ndisc galaxies in the near-infrared using the Ha emission line in order to study\nthe Tully-Fisher relation. To put any observed evolution into perspective and\nto investigate any possible selection biases, we constructed a control sample\nof low redshift galaxies that had rotation velocities and images available for\nmeasuring their dynamical, photometric, and morphological properties. Compared\nto local objects with isophotal sizes similar to the high redshift targets, we\nfind that our sample of galaxies with spatially resolved rotation curves, the\nmost distant sample so far (\u003Cz\u003E~0.9), clearly reveals a brightening of ~1.1 mag\nin the rest-frame B-band. The observed offset can be explained by a combination\nof increasing surface brightness, decreasing rotation speeds, and slightly\nsmaller disc scale lengths of the high redshift galaxies.","abstract_zh":"","authors":[{"id":"54054057dabfae8faa5b8a04","name":"M. Barden"},{"id":"5607c86645cedb3396b65a89","name":"M. D. Lehnert"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"5607c86645cedb3396b65a8c","name":"R. Genzel"},{"id":"5607c86645cedb3396b65a8f","name":"S. White"},{"id":"53f45d91dabfaee02ad72c2d","name":"A. Franceschini"}],"doi":"","id":"53e9aecbb7602d97038f1107","lang":"en","num_citation":5,"order":2,"pages":{"end":"","start":""},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F03\u002F0302\u002Fastro-ph0302392.pdf","title":"Ha Rotation Curves of z~1 Galaxies: Unraveling the Evolution of the Tully-Fisher Relation","urls":["https:\u002F\u002Farxiv.org\u002Fabs\u002Fastro-ph\u002F0302392"],"venue":{"issue":"","volume":""},"versions":[{"id":"53e2806c20f7fff67832b272","sid":"27786505","src":"msra","year":2003},{"id":"56d88a69dabfae2eeeb1afb7","sid":"1511734622","src":"mag","year":2003},{"id":"5c750154f56def979849e40c","sid":"1511734622","src":"mag","vsid":"2595170531","year":2003},{"id":"5c6109cada56297340b8fecc","sid":"astro-ph\u002F0302392","src":"arxiv","year":2003}],"year":2003},{"abstract":"We have used the IRAM Plateau de Bure millimeter interferometer to locate with subarcsecond accuracy the dust emission of three of the brightest 1.2 mm sources in the NTT Deep Field selected from our 1.2 mm Max-Planck-Millimeter Bolometer Array survey at the IRAM 30 m telescope. We combine these results with deep B to K imaging and Very Large Array interferometry. Reliable identifications are an essential step toward an understanding of the high-redshift (sub) millimeter galaxy population, toward testing the common belief that they are scaled-up analogs of local dusty ultraluminous galaxies, and in shedding light on the possible connection to spheroid formation. Strikingly, none of the three accurately located millimeter galaxies MM J120546-0741.5, MM J120539-0745.4, and MM J120517-0743.1 has a K-band counterpart down to the faint limit of K-s \u003E 21.9. This implies that these three galaxies either are extremely obscured and\u002For are at very high redshifts (z greater than or similar to 4). We combine our results with literature data for 11 more (sub) millimeter galaxies that are identified with similar reliability. In terms of their K-band properties, the sample divides into three roughly equal groups: (1) undetected to K similar to 22, (2) detected in the near-infrared but not the optical, and (3) detected in the optical with the possibility of optical follow-up spectroscopy. We find a trend in this sample between near-infrared to submillimeter and submillimeter to radio spectral indexes, which in comparison to spectral energy distributions (SEDs) of low-redshift infrared-luminous galaxies suggests that the most plausible primary factor causing the extreme near-infrared faintness of our objects is their high redshift. We show that the near-infrared to radio SEDs of the sample are inconsistent with SEDs that resemble local far-infrared cool galaxies with moderate luminosities, which were proposed in some models of the submillimeter sky. We briefly discuss the implications of the results for our understanding of galaxy formation.","authors":[{"id":"53f4460bdabfaedd74decc15","name":"H. Dannerbauer"},{"id":"560c16cd45cedb3397488556","name":"M. D. Lehnert"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"544820d1dabfae87b7ddcaef","name":"F. Bertoldi"},{"id":"53f47371dabfaedd74e9d2e6","name":"C. Carilli"},{"id":"560c59dc45cedb3397523d9e","name":"R. Genzel"},{"id":"53f42f92dabfaee0d9b18913","name":"K. Menten"}],"doi":"10.1086\u002F340762","id":"53e9a711b7602d9703049fdd","lang":"en","num_citation":0,"order":3,"pages":{"end":"484","start":"473"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F02\u002F0201\u002Fastro-ph0201104.pdf","title":"Properties of Millimeter Galaxies: Constraints from\u003Ci\u003EK\u003C\u002Fi\u003E‐Band Blank Fields","venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"573"},"versions":[{"id":"53e2b5e620f7fff6791a3ec0","sid":"43149985","src":"msra","year":2002},{"id":"5c6109c1da56297340b8dced","sid":"astro-ph\u002F0201104","src":"arxiv","year":2002},{"id":"5fd56137a4e4c3c831871116","sid":"WOS:000176663000001","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2002}],"year":2002},{"abstract":"We have used the IRAM Plateau de Bure millimeter interferometer to locate with subarcsecond accuracy the dust emission of three of the brightest 1.2 mm sources in the NTT Deep Field selected from our 1.2 mm Max-Planck-Millimeter Bolometer Array survey at the IRAM 30 m telescope. We combine these results with deep B to K imaging and Very Large Array interferometry. Reliable identifications are an essential step toward an understanding of the high-redshift (sub) millimeter galaxy population, toward testing the common belief that they are scaled-up analogs of local dusty ultraluminous galaxies, and in shedding light on the possible connection to spheroid formation. Strikingly, none of the three accurately located millimeter galaxies MM J120546-0741.5, MM J120539-0745.4, and MM J120517-0743.1 has a K-band counterpart down to the faint limit of K-s \u003E 21.9. This implies that these three galaxies either are extremely obscured and\u002For are at very high redshifts (z greater than or similar to 4). We combine our results with literature data for 11 more (sub) millimeter galaxies that are identified with similar reliability. In terms of their K-band properties, the sample divides into three roughly equal groups: (1) undetected to K similar to 22, (2) detected in the near-infrared but not the optical, and (3) detected in the optical with the possibility of optical follow-up spectroscopy. We find a trend in this sample between near-infrared to submillimeter and submillimeter to radio spectral indexes, which in comparison to spectral energy distributions (SEDs) of low-redshift infrared-luminous galaxies suggests that the most plausible primary factor causing the extreme near-infrared faintness of our objects is their high redshift. We show that the near-infrared to radio SEDs of the sample are inconsistent with SEDs that resemble local far-infrared cool galaxies with moderate luminosities, which were proposed in some models of the submillimeter sky. We briefly discuss the implications of the results for our understanding of galaxy formation.","abstract_zh":"","authors":[{"id":"53f4460bdabfaedd74decc15","name":"H. Dannerbauer"},{"id":"54872c7bdabfae9b401342ca","name":"M. D. Lehnert"},{"id":"5434ea82dabfaebba587d892","name":"D. Lutz"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"544820d1dabfae87b7ddcaef","name":"F. Bertoldi"},{"name":"C. Carilli"},{"id":"560c59dc45cedb3397523d9e","name":"R. Genzel"},{"id":"53f42f92dabfaee0d9b18913","name":"K. Menten"}],"doi":"10.1086\u002F340762","id":"53e9a72eb7602d9703067457","lang":"en","num_citation":78,"order":3,"pages":{"end":"484","start":"473"},"pdf":"https:\u002F\u002Fstatic.aminer.cn\u002Fstorage\u002Fpdf\u002Farxiv\u002F02\u002F0201\u002Fastro-ph0201104.pdf","title":"Properties of mm galaxies: Constraints from K-band blank fields","urls":["http:\u002F\u002Fdx.doi.org\u002F10.1086\u002F340762","https:\u002F\u002Farxiv.org\u002Fabs\u002Fastro-ph\u002F0201104","http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTROPHYSICAL JOURNAL"},"issue":"2","volume":"573"},"versions":[{"id":"53e2633420f7fff677980d49","sid":"12556615","src":"msra","year":2002},{"id":"56d83784dabfae2eee4a31ac","sid":"2032627069","src":"mag","year":2002},{"id":"5c6109c1da56297340b8dced","sid":"astro-ph\u002F0201104","src":"arxiv","year":2002},{"id":"5fd56137a4e4c3c831871116","sid":"WOS:000176663000001","src":"wos","vsid":"ASTROPHYSICAL JOURNAL","year":2002}],"year":2002},{"abstract":"We report 0.5 \" resolution imaging of the Cloverleaf quasar in the CO(7-6) line and 1.3 mm continuum,, as well as 1 \" resolution imaging in the CO(3-2) line, performed with the IRAM interferometer. The CO(7-6) image is clearly resolved into 4 spots, demonstrating that the CO emission is also gravitationally lensed. We do not find any convincing evidence for a velocity gradient in the maps. As compared to the optical spots from a V band HST image, some of the CO spots are found to be stretched along the Einstein ring. Using the available lens model for the Cloverleaf, this suggests an intrinsic radius of similar to 600 pc for the CO emitting region. No continuum emission is detected: the measured flux density is 5 +\u002F- 3 mJy, consistent with a spectral index larger than 3.","abstract_zh":"","authors":[{"id":"53f43101dabfaedd74d64f53","name":"D. Alloin"},{"id":"53f430c0dabfaee4dc743f9c","name":"S. Guilloteau"},{"id":"53f433d4dabfaec09f164071","name":"R. Barvainis"},{"id":"5448b6bedabfae87b7e6a37b","name":"R. Antonucci"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"}],"doi":"","id":"53e9ba1cb7602d970462075b","lang":"en","num_citation":0,"order":4,"pages":{"end":"28","start":"24"},"title":"The gravitational lensing nature of the Cloverleaf unveiled in CO (7-6) line emission?","urls":["http:\u002F\u002Fwww.webofknowledge.com\u002F"],"venue":{"info":{"name":"ASTRONOMY & ASTROPHYSICS"},"issue":"1","volume":"321"},"versions":[{"id":"53e25ee320f7fff677863a3d","sid":"10980118","src":"msra","year":0},{"id":"56d91f5adabfae2eee93ffac","sid":"62003285","src":"mag","year":1997},{"id":"5fc6f677d75e2ac63d578709","sid":"WOS:A1997XB42000008","src":"wos","vsid":"ASTRONOMY & ASTROPHYSICS","year":1997}],"year":1997},{"abstract":"We describe the first results of a programme to obtain rotation curves of z ≈ 1 disc galaxies in the near-infrared using the Hemission line in order to study the Tully-Fisher relationship. To put any observed evolution into perspective and to investigate any possible selection biases, we constructed a control sample of low redshift galaxies that had rotation velocities and images available for measuring their dynamical, photometric, and morphological properties. Compared to local objects with isophotal sizes similar to the high redshift targets, we find that our sample of galaxies with spatially resolved rotation curves, the most distant sample so far (h zi ≈ 0.9), clearly reveals a brightening of ≈ 1.1 mag in the rest-frame B-band. The observed offset can be explained by a combination of increasing surface brightness, decreasing rotation speeds, and slightly smaller disc scale lengths of the high redshift galaxies.","authors":[{"id":"54054057dabfae8faa5b8a04","name":"M. Barden"},{"id":"560895ac45cedb3396d0b039","name":"M. D. Lehnert"},{"id":"53f7d14ddabfae8faa4b843e","name":"L. Tacconi"},{"id":"560895ac45cedb3396d0b03c","name":"R. Genzel"},{"id":"560895ac45cedb3396d0b03f","name":"S. White"},{"id":"53f45d91dabfaee02ad72c2c","name":"A. Franceschini"}],"doi":"","id":"53e9b189b7602d9703c11891","lang":"en","num_citation":0,"order":2,"pdf":"","title":"HRotation Curves of z ∼ 1 Galaxies: Unraveling the Evolution of the Tully-Fisher Relation1","versions":[{"id":"53e2631920f7fff677978968","sid":"12519044","src":"msra","year":0}],"year":0}],"profilePubsTotal":17,"profilePatentsPage":1,"profilePatents":[],"profilePatentsTotal":0,"profilePatentsEnd":true,"profileProjectsPage":0,"profileProjects":null,"profileProjectsTotal":null,"newInfo":null,"checkDelPubs":[]}};