https://tel.archives-ouvertes.fr/file/index/docid/1058049/filename/HOU_XIAN_2013.pdf
... year of my thesis and in my job hunting, though we haven’t really chatted much in the real world, incredible! I will not forget to express my appreciation to the Pulsar Timing Consortium which has generously provided radio ephemerides for pulsars without which my detections of gamma-ray pulsars woul ...
... year of my thesis and in my job hunting, though we haven’t really chatted much in the real world, incredible! I will not forget to express my appreciation to the Pulsar Timing Consortium which has generously provided radio ephemerides for pulsars without which my detections of gamma-ray pulsars woul ...
arXiv:astro-ph/0702414v1 15 Feb 2007
... plane. All data were collected in service mode using one single MXU mask for each grism. The FORS2 detector, which consists of two 2k × 4k MIT CCDs, was used in the 100kHz readout mode with high gain. A 2×2 binning was performed during the readout. The observations with the 1400V grism were carried ...
... plane. All data were collected in service mode using one single MXU mask for each grism. The FORS2 detector, which consists of two 2k × 4k MIT CCDs, was used in the 100kHz readout mode with high gain. A 2×2 binning was performed during the readout. The observations with the 1400V grism were carried ...
The XMM-Newton Bright Serendipitous Survey
... The identification of the optical counterparts of the XBS sources is relatively easy given the combination of the good positions of the XMM-Newton sources (90% error ∼400 , Della Ceca et al. 2004) and the brightness of the sources: X-ray sources with FX >10−13 erg cm−2 s−1 are expected to have an op ...
... The identification of the optical counterparts of the XBS sources is relatively easy given the combination of the good positions of the XMM-Newton sources (90% error ∼400 , Della Ceca et al. 2004) and the brightness of the sources: X-ray sources with FX >10−13 erg cm−2 s−1 are expected to have an op ...
Discovery and Study of Exotic Radio Pulsars Jason William Thomas
... and determine their luminosity distribution. This survey and the follow-up studies of our discoveries were a major undertaking, which required 6 proposals to the Arecibo observatory and over 400 hr of observations with the Arecibo telescope. I have been involved in this project since the very first o ...
... and determine their luminosity distribution. This survey and the follow-up studies of our discoveries were a major undertaking, which required 6 proposals to the Arecibo observatory and over 400 hr of observations with the Arecibo telescope. I have been involved in this project since the very first o ...
PhD thesis
... 3.3.2 Spectral energy distribution . . . . . . . . . . . . . . . . . . . 3.4 Molecular results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3.4.1 Molecular dense gas: morphology and velocity fields . . . . . 3.4.2 Molecular dense gas: temperature and density . . . . . . . . 3.4.3 Ionize ...
... 3.3.2 Spectral energy distribution . . . . . . . . . . . . . . . . . . . 3.4 Molecular results . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 3.4.1 Molecular dense gas: morphology and velocity fields . . . . . 3.4.2 Molecular dense gas: temperature and density . . . . . . . . 3.4.3 Ionize ...
A Multi-wavelength study on gamma
... Dr. Bing Zhang, Examination Committee Chair Professor of Physics University of Nevada, Las Vegas During the prompt emission and afterglow phases, GRBs(Gamma-Ray Bursts) release their huge amount of energy not limited in gamma-ray, but in a wide range of mutiwavelengths, from radio band to GeV gamma- ...
... Dr. Bing Zhang, Examination Committee Chair Professor of Physics University of Nevada, Las Vegas During the prompt emission and afterglow phases, GRBs(Gamma-Ray Bursts) release their huge amount of energy not limited in gamma-ray, but in a wide range of mutiwavelengths, from radio band to GeV gamma- ...
Link - Max-Planck-Institut für Astronomie
... examples of this phenomenon. FUors are believed to undergo accretion outbursts during which the accretion rate rapidly increases from typically 10−7 to a few 10−4 M⊙ yr−1 , and remains elevated over several decades or more. EXors, a loosely defined class of pre-main sequence stars, exhibit shorter a ...
... examples of this phenomenon. FUors are believed to undergo accretion outbursts during which the accretion rate rapidly increases from typically 10−7 to a few 10−4 M⊙ yr−1 , and remains elevated over several decades or more. EXors, a loosely defined class of pre-main sequence stars, exhibit shorter a ...
arXiv:1410.8731v2 [astro
... all measurements and plots are derived from the higher quality data cube. Flux calibration was done using aperture photometry on a deconvolved K-band image created from the final data cube. The deconvolution was performed using the Lucy-Richardson algorithm incorporated in DPUSER, while the PSF was ...
... all measurements and plots are derived from the higher quality data cube. Flux calibration was done using aperture photometry on a deconvolved K-band image created from the final data cube. The deconvolution was performed using the Lucy-Richardson algorithm incorporated in DPUSER, while the PSF was ...
Andrea Santangelo
... Accretion though at much lower luminosity is there! We possibly observe the inhibition of the column at lower luminosities: radiation comes from the polar cap In “the gated accretion” scenario of Bozzo+ (2008), we might see here the transition to KH Instab. ...
... Accretion though at much lower luminosity is there! We possibly observe the inhibition of the column at lower luminosities: radiation comes from the polar cap In “the gated accretion” scenario of Bozzo+ (2008), we might see here the transition to KH Instab. ...
Dust in historical Galactic Type Ia supernova remnants with Herschel
... of the warm dust with X-rays from the ejecta and swept-up medium, and Hα emission arising from the post-shock edge, we show that the warm dust is swept up interstellar material. We find no evidence of a cool (25–50 K) component of dust with mass ≥0.07 M as observed in core-collapse remnants of mass ...
... of the warm dust with X-rays from the ejecta and swept-up medium, and Hα emission arising from the post-shock edge, we show that the warm dust is swept up interstellar material. We find no evidence of a cool (25–50 K) component of dust with mass ≥0.07 M as observed in core-collapse remnants of mass ...
Some Constraints on the Effects of Age and Metallicity - UvA-DARE
... consider only the X-ray sources that lie within the WFPC2 field of view. Thirty-six of the LMXB candidates in NGC 3115 and 44 in NGC 4365 meet this criterion (we eliminated the source corresponding to the nucleus of each galaxy, which may be associated with their central black holes). Nine of these ...
... consider only the X-ray sources that lie within the WFPC2 field of view. Thirty-six of the LMXB candidates in NGC 3115 and 44 in NGC 4365 meet this criterion (we eliminated the source corresponding to the nucleus of each galaxy, which may be associated with their central black holes). Nine of these ...
Probing nuclear activity versus star formation at z ∼ 0.8 using near
... selected sources at a median redshift of z ∼ 0.8 in the Extended Groth Strip (EGS). To date this is the largest compilation of NIR spectra of active galactic nuclei (AGN) at this redshift. The data were obtained using the multi-object spectroscopic mode of the Long-slit Intermediate Resolution Infra ...
... selected sources at a median redshift of z ∼ 0.8 in the Extended Groth Strip (EGS). To date this is the largest compilation of NIR spectra of active galactic nuclei (AGN) at this redshift. The data were obtained using the multi-object spectroscopic mode of the Long-slit Intermediate Resolution Infra ...
LARGE-SCALE EXTENDED EMISSION AROUND THE HELIX
... We present new observations of the ionized gas, molecular gas, and cool dust in the Helix Nebula (NGC 7293). The ionized gas is observed in the form of an H image, which is constructed using images from the Southern H Sky Survey Atlas. The molecular emission was mapped using the H2 v = 1 ! 0 S(1) ...
... We present new observations of the ionized gas, molecular gas, and cool dust in the Helix Nebula (NGC 7293). The ionized gas is observed in the form of an H image, which is constructed using images from the Southern H Sky Survey Atlas. The molecular emission was mapped using the H2 v = 1 ! 0 S(1) ...
Multiwavelength optical observations of chromospherically active
... camera Astromed-3200 and a 1152 × 770 pixel EEV P88200 CCD detector. The wavelength range covers from 3765 to 9865 Å, for the first run, and from 3632 to 10 800 Å, for the second run. The reciprocal dispersion ranges from 0.07 to 0.18 Å/pixel and the spectral resolution, determined as the full wi ...
... camera Astromed-3200 and a 1152 × 770 pixel EEV P88200 CCD detector. The wavelength range covers from 3765 to 9865 Å, for the first run, and from 3632 to 10 800 Å, for the second run. The reciprocal dispersion ranges from 0.07 to 0.18 Å/pixel and the spectral resolution, determined as the full wi ...
the PDF program book
... Reserve a Meeting Room There are five meeting rooms in UKK (rooms K1 – K4, K6) that may be used for meetings or telecons. The rooms are located on level 3 and seat between 12 and 24 people. If you want to hold a small meeting, you can either speak to the LOC representative at the registration desk o ...
... Reserve a Meeting Room There are five meeting rooms in UKK (rooms K1 – K4, K6) that may be used for meetings or telecons. The rooms are located on level 3 and seat between 12 and 24 people. If you want to hold a small meeting, you can either speak to the LOC representative at the registration desk o ...
Revising the census of low luminosity AGN
... WHY AN AGN CENSUS? • A PROPER AGN CENSUS IS NEEDED FOR A VARIETY OF STUDIES, SUCH AS, E.G. , THE AGN/HOST GALAXY CONNECTION, THE PROPERTIES OF THE CENTRAL ENGINE, THE AGN LUMINOSITY FUNCTION … • THE CENSUS SHOULD BE COMPLETE (OR AT LEAST WITH WELL DEFINED BIASES) AND INCLUDE THE LEAST NUMBER OF INT ...
... WHY AN AGN CENSUS? • A PROPER AGN CENSUS IS NEEDED FOR A VARIETY OF STUDIES, SUCH AS, E.G. , THE AGN/HOST GALAXY CONNECTION, THE PROPERTIES OF THE CENTRAL ENGINE, THE AGN LUMINOSITY FUNCTION … • THE CENSUS SHOULD BE COMPLETE (OR AT LEAST WITH WELL DEFINED BIASES) AND INCLUDE THE LEAST NUMBER OF INT ...
Multiple Jets from the High-Mass (Proto) stellar Cluster AFGL5142
... heating implied by the temperature indicates that MM-1 and MM-2 cores contain embedded massive young stars. Additional dust continuum peaks MM-4 and MM-5 appear to be associated with H2 O masers. With many continuum sources at cm and mm wavelengths, and those already identified in the infrared, this ...
... heating implied by the temperature indicates that MM-1 and MM-2 cores contain embedded massive young stars. Additional dust continuum peaks MM-4 and MM-5 appear to be associated with H2 O masers. With many continuum sources at cm and mm wavelengths, and those already identified in the infrared, this ...
as a PDF - Living Reviews in Solar Physics
... flares) are key factors in the formation and evolution of the planets and eventually the biosphere on Earth. The Sun is, like almost all cool stars, a “magnetic star” that produces magnetic fields through dynamo operation in the interior. These fields reach the surface where their presence is notice ...
... flares) are key factors in the formation and evolution of the planets and eventually the biosphere on Earth. The Sun is, like almost all cool stars, a “magnetic star” that produces magnetic fields through dynamo operation in the interior. These fields reach the surface where their presence is notice ...
Spitzer Spectroscopy of Circumstellar Disks in the 5 Myr Old Upper
... emission in excess of photospheric values at 8 or 16 µm. The low-mass (0.1–1.2 M⊙ ) stars are associated with excess emission that is characteristic of optically thick disks found around classical T Tauri stars. Stars more massive than ∼1.8 M⊙ are found with weak excesses at short wavelengths indica ...
... emission in excess of photospheric values at 8 or 16 µm. The low-mass (0.1–1.2 M⊙ ) stars are associated with excess emission that is characteristic of optically thick disks found around classical T Tauri stars. Stars more massive than ∼1.8 M⊙ are found with weak excesses at short wavelengths indica ...
Article PDF - IOPscience
... lines, H2 gas, polycyclic aromatic hydrocarbon (PAH) emission, warm dust from T = 50 to 150 K, and silicate features in both emission and absorption. There is no evidence in the mid-IR of a single template for CSO hosts, but 5/8 galaxies show similar moderate levels of star formation (<10 M yr−1 fr ...
... lines, H2 gas, polycyclic aromatic hydrocarbon (PAH) emission, warm dust from T = 50 to 150 K, and silicate features in both emission and absorption. There is no evidence in the mid-IR of a single template for CSO hosts, but 5/8 galaxies show similar moderate levels of star formation (<10 M yr−1 fr ...
Astronomy
... originate outside the Earth's atmosphere (such as the cosmic background radiation). It is concerned with the evolution, physics, chemistry, meteorology, and motion of celestial objects, as well as the formation and development of the universe. Astronomy is one of the oldest sciences. Prehistoric cul ...
... originate outside the Earth's atmosphere (such as the cosmic background radiation). It is concerned with the evolution, physics, chemistry, meteorology, and motion of celestial objects, as well as the formation and development of the universe. Astronomy is one of the oldest sciences. Prehistoric cul ...
Annual Report 2014 - Max Planck Institute for Astrophysics
... 2.3 An observational and theoretical view of the atomic gas distribution in galaxies . . . . . 2.4 New analytical model for turbulence pressure in galaxy clusters . . . . . . . . . . . . . . 2.5 Resolving the radio sky . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.6 Stell ...
... 2.3 An observational and theoretical view of the atomic gas distribution in galaxies . . . . . 2.4 New analytical model for turbulence pressure in galaxy clusters . . . . . . . . . . . . . . 2.5 Resolving the radio sky . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2.6 Stell ...
X-ray binaries in the Milky Way and other galaxies
... 6.1. Universal HMXB Luminosity Function ? . . . . . . . . . . . . . . . . . . . 6.2. High Luminosity cut-off . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.3. Total X-ray luminosity as SFR indicator . . . . . . . . . . . . . . . . . . . 6.4. Theoretical LX –SFR relation . . . . . . . . . ...
... 6.1. Universal HMXB Luminosity Function ? . . . . . . . . . . . . . . . . . . . 6.2. High Luminosity cut-off . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6.3. Total X-ray luminosity as SFR indicator . . . . . . . . . . . . . . . . . . . 6.4. Theoretical LX –SFR relation . . . . . . . . . ...
Accreting millisecond X-ray pulsars, from accretion disk to magnetic
... of the first X-ray satellite UHURU, it became clear that Sco X-1 belonged to a more general and extended family of X-ray binary sources with a compact accretor stripping gas from a canonical star. Since then, the number of known neutron stars has increased enormously and neutron stars have been obse ...
... of the first X-ray satellite UHURU, it became clear that Sco X-1 belonged to a more general and extended family of X-ray binary sources with a compact accretor stripping gas from a canonical star. Since then, the number of known neutron stars has increased enormously and neutron stars have been obse ...
Massive Disruptions in the Cool Core of MACS J1931.8-2634 Steven Ehlert
... Snowcluster March 31st 2010 ...
... Snowcluster March 31st 2010 ...
X-ray astronomy
X-ray astronomy is an observational branch of astronomy which deals with the study of X-ray observation and detection from astronomical objects. X-radiation is absorbed by the Earth's atmosphere, so instruments to detect X-rays must be taken to high altitude by balloons, sounding rockets, and satellites. X-ray astronomy is the space science related to a type of space telescope that can see farther than standard light-absorption telescopes, such as the Mauna Kea Observatories, via x-ray radiation.X-ray emission is expected from astronomical objects that contain extremely hot gasses at temperatures from about a million kelvin (K) to hundreds of millions of kelvin (MK). Although X-rays have been observed emanating from the Sun since the 1940s, the discovery in 1962 of the first cosmic X-ray source was a surprise. This source is called Scorpius X-1 (Sco X-1), the first X-ray source found in the constellation Scorpius. The X-ray emission of Scorpius X-1 is 10,000 times greater than its visual emission, whereas that of the Sun is about a million times less. In addition, the energy output in X-rays is 100,000 times greater than the total emission of the Sun in all wavelengths. Based on discoveries in this new field of X-ray astronomy, starting with Scorpius X-1, Riccardo Giacconi received the Nobel Prize in Physics in 2002. It is now known that such X-ray sources as Sco X-1 are compact stars, such as neutron stars or black holes. Material falling into a black hole may emit X-rays, but the black hole itself does not. The energy source for the X-ray emission is gravity. Infalling gas and dust is heated by the strong gravitational fields of these and other celestial objects.Many thousands of X-ray sources are known. In addition, the space between galaxies in galaxy clusters is filled with a very hot, but very dilute gas at a temperature between 10 and 100 megakelvins (MK). The total amount of hot gas is five to ten times the total mass in the visible galaxies.