Into the sub-mm
... Andrew Blain (MRAO) followed with a discussion of the results of a SCUBA pilot survey for previously unknown galaxies. The results and implications of Smail, Ivison and Blain’s observations of distant lensing clusters, revealing the first sub-millimetre selected objects (including a redshift 2 galax ...
... Andrew Blain (MRAO) followed with a discussion of the results of a SCUBA pilot survey for previously unknown galaxies. The results and implications of Smail, Ivison and Blain’s observations of distant lensing clusters, revealing the first sub-millimetre selected objects (including a redshift 2 galax ...
NGC 1808 - Rencontres de Moriond
... + The contribution to soft X-rays might be non-negligible, but is is any case below 30%. + The contribution to hard X-rays is negligible. + The SSC could produce only around 1/50 of the ionizing photons producing the observed emission line spectrum, and no more than 1/10 of the observed FIR luminosi ...
... + The contribution to soft X-rays might be non-negligible, but is is any case below 30%. + The contribution to hard X-rays is negligible. + The SSC could produce only around 1/50 of the ionizing photons producing the observed emission line spectrum, and no more than 1/10 of the observed FIR luminosi ...
color-stellar mass diagram
... luminosity, mass, color, morphology, stellar population of galaxies are strongly related. analysis of such properties in the cosmic time started first with the study of the luminosity function but later included galaxy counts as function of the various parameters however, almost all these properties ...
... luminosity, mass, color, morphology, stellar population of galaxies are strongly related. analysis of such properties in the cosmic time started first with the study of the luminosity function but later included galaxy counts as function of the various parameters however, almost all these properties ...
Starburst Galaxies Under the Microscope: High
... Starburst galaxies are unique laboratories. Starburst episodes are phases in the evolution of galaxies that are by definition transient, and during which they convert a significant fraction of their gas reservoirs into stars. During a starburst phase a galaxy thus evolves rapidly in stellar, gas, du ...
... Starburst galaxies are unique laboratories. Starburst episodes are phases in the evolution of galaxies that are by definition transient, and during which they convert a significant fraction of their gas reservoirs into stars. During a starburst phase a galaxy thus evolves rapidly in stellar, gas, du ...
Collaborations with East Asian VLBI stations
... Target sources : Galactic masers (H2O@22GHz, SiO@43GHz) New aspect: dual-beam for phase-referencing ...
... Target sources : Galactic masers (H2O@22GHz, SiO@43GHz) New aspect: dual-beam for phase-referencing ...
So, what`s the problem for high
... far-IR (50-200m), dust emission gives virtually total luminosity (power in watts). In millimeter and submillimeter wavelengths, dust emission can be used to measure the mass of a molecular cloud, and its star forming cores. ...
... far-IR (50-200m), dust emission gives virtually total luminosity (power in watts). In millimeter and submillimeter wavelengths, dust emission can be used to measure the mass of a molecular cloud, and its star forming cores. ...
The Strikingly Uniform, Highly Turbulent Interstellar Medium of the
... awarded 8.1h in bands 7 and 8 to study the red-shifted 157.7µm (2 P3/2 → 2 P1/2 ) fine-structure transition of ionized carbon, [C ii], and the underlying dust continuum emission in a sample of Hot DOGs spanning a range of redshifts and luminosities. Observations of W2246-0526, the first galaxy of th ...
... awarded 8.1h in bands 7 and 8 to study the red-shifted 157.7µm (2 P3/2 → 2 P1/2 ) fine-structure transition of ionized carbon, [C ii], and the underlying dust continuum emission in a sample of Hot DOGs spanning a range of redshifts and luminosities. Observations of W2246-0526, the first galaxy of th ...
Active Galaxies
... Active galaxies have an energy source beyond what can be attributed to stars. The energy is believed to originate from accretion onto a supermassive blackhole. Active galaxies tend to have higher overall luminosities and very different spectra than “normal” galaxies. “non-stellar” radiation ...
... Active galaxies have an energy source beyond what can be attributed to stars. The energy is believed to originate from accretion onto a supermassive blackhole. Active galaxies tend to have higher overall luminosities and very different spectra than “normal” galaxies. “non-stellar” radiation ...
Searching for Dwarf Galaxies and Population III Star
... This multi-step project includes 3 tiers of observations: 1. By 2016, the James Webb Space Telescope will regularly deliver deep infrared images that reveal the most massive star-forming galaxies and proto-clusters of galaxies at z > 7. We will identify the most luminous at z ~ 7.7, where Lyman fa ...
... This multi-step project includes 3 tiers of observations: 1. By 2016, the James Webb Space Telescope will regularly deliver deep infrared images that reveal the most massive star-forming galaxies and proto-clusters of galaxies at z > 7. We will identify the most luminous at z ~ 7.7, where Lyman fa ...
Does size matter (in the SFRs)?
... sented the results on the SFRs of two small spiral galaxies with very similar HI content but with different size. According to Kennicutt (1998) they both should be galaxies are more the same locations of the graph, and have very similar values of the SFRs. On the contrary of course, UGC 5296 is not ...
... sented the results on the SFRs of two small spiral galaxies with very similar HI content but with different size. According to Kennicutt (1998) they both should be galaxies are more the same locations of the graph, and have very similar values of the SFRs. On the contrary of course, UGC 5296 is not ...
main characteristics of the emission from elliptical galaxies
... Now, a star is hardly an object at thermal equilibrium, in fact the temperature decreases steeply from the core to the photosphere. Fortunately we can always consider shells or layers small enough where a Local Thermodynamic Equilibrium is established: uctuations in T within each layer can happen, ...
... Now, a star is hardly an object at thermal equilibrium, in fact the temperature decreases steeply from the core to the photosphere. Fortunately we can always consider shells or layers small enough where a Local Thermodynamic Equilibrium is established: uctuations in T within each layer can happen, ...
Galactic Parameters from Masers with Trigonometric Parallaxes
... located in the range of galactocentric distances 3
... located in the range of galactocentric distances 3
Classification and structure of galaxies
... • has about 200 billion stars, and lots of gas and dust • is a barred-spiral (we think) • about 100,000 light-years wide • our Sun is halfway to the edge, revolving at half a million miles per hour around the center of the Galaxy • takes our Solar System about 200 million years to revolve once aroun ...
... • has about 200 billion stars, and lots of gas and dust • is a barred-spiral (we think) • about 100,000 light-years wide • our Sun is halfway to the edge, revolving at half a million miles per hour around the center of the Galaxy • takes our Solar System about 200 million years to revolve once aroun ...
6.7 GHz Methanol Masers and the GBT
... • Most telescopes in U.S. currently do not have the capability to observe between 6 and 8 GHz of CBand. • This band includes the 6030 and 6035 MHz OH lines and the 6668 GHz line of methanol. • The latter is a very strong maser line observed in Galactic star forming regions. ...
... • Most telescopes in U.S. currently do not have the capability to observe between 6 and 8 GHz of CBand. • This band includes the 6030 and 6035 MHz OH lines and the 6668 GHz line of methanol. • The latter is a very strong maser line observed in Galactic star forming regions. ...
z - STScI
... – Angular resolution and wide field to survey 100,000 protogalaxies and their environments (to z ~ 5) – mid infrared imaging and spectroscopy to pinpoint the nature of the hidden stars and Active Galactic Nuclei ...
... – Angular resolution and wide field to survey 100,000 protogalaxies and their environments (to z ~ 5) – mid infrared imaging and spectroscopy to pinpoint the nature of the hidden stars and Active Galactic Nuclei ...
Interstellar Medium and Star Formation
... Substantial additional mass discovered with detection of molecular lines from dense gas Millimeter wavelengths for rotational, vibrational lines from heterogeneous molecules NH2 and H2O first found (Cheung et al. 1968, Knowles et al. 1969) then CO (Penzias et al. 1970), used to trace H2 Supert ...
... Substantial additional mass discovered with detection of molecular lines from dense gas Millimeter wavelengths for rotational, vibrational lines from heterogeneous molecules NH2 and H2O first found (Cheung et al. 1968, Knowles et al. 1969) then CO (Penzias et al. 1970), used to trace H2 Supert ...
Quasars - Ann Arbor Earth Science
... increasing separation between the core and a knot in the jet) which appears faster than the speed of light in our frame of reference. The data are consistent with this being a transformation effect from seeing jets moving almost directly toward us, so that the emitting material almost catches up wit ...
... increasing separation between the core and a knot in the jet) which appears faster than the speed of light in our frame of reference. The data are consistent with this being a transformation effect from seeing jets moving almost directly toward us, so that the emitting material almost catches up wit ...
1 Research Experience for Cara Battersby I include very briefly here
... This paper has a simple goal: to estimate the lifetimes of two evolutionary phases in the formation of stellar clusters. These phases are the cold dense pre-cluster-clump (PCC) phase and the warm, diffuse, actively star-forming clump phase, as identified by Battersby et al. (2011). We use the Hersch ...
... This paper has a simple goal: to estimate the lifetimes of two evolutionary phases in the formation of stellar clusters. These phases are the cold dense pre-cluster-clump (PCC) phase and the warm, diffuse, actively star-forming clump phase, as identified by Battersby et al. (2011). We use the Hersch ...
- ORIGINS Space Telescope
... Joaquin Vieira (University of Illinois) for the Origins Space Telescope Science and Technology Definition Team ABSTRACT — The Origins Space Telescope (OST) is the mission concept for the Far-Infrared Surveyor, a study in development by NASA in preparation for the 2020 Astronomy and Astrophysics Deca ...
... Joaquin Vieira (University of Illinois) for the Origins Space Telescope Science and Technology Definition Team ABSTRACT — The Origins Space Telescope (OST) is the mission concept for the Far-Infrared Surveyor, a study in development by NASA in preparation for the 2020 Astronomy and Astrophysics Deca ...
Joining the Party - Lincoln-Sudbury Regional High School
... These explosions are likely to keep on happening, but we can’t predict when. ...
... These explosions are likely to keep on happening, but we can’t predict when. ...
TF_final3 - Arecibo Observatory
... i in infrared. The TullyFisher relation states that the bigger the galaxy is, the faster it rotates. The faster the galaxy rotates, the wider is the emission line in velocity. Also, the bigger the galaxy, the more is its luminosity. TullyFisher relation shows that for normal galaxies, the velocity w ...
... i in infrared. The TullyFisher relation states that the bigger the galaxy is, the faster it rotates. The faster the galaxy rotates, the wider is the emission line in velocity. Also, the bigger the galaxy, the more is its luminosity. TullyFisher relation shows that for normal galaxies, the velocity w ...
Extragalactic AO Science
... Sensitivity increases rapidly with Strehl for point sources, but extended targets gain much less. AO systems produce additional background in Near-IR and reduce throughput further making it difficult to observe faint extended sources. Normal galaxy disks only achieve a maximum SB of K~16 mag/sq arcs ...
... Sensitivity increases rapidly with Strehl for point sources, but extended targets gain much less. AO systems produce additional background in Near-IR and reduce throughput further making it difficult to observe faint extended sources. Normal galaxy disks only achieve a maximum SB of K~16 mag/sq arcs ...
The galaxies that host powerful radio sources
... What do we know about these sources: Sub-mm flux combined with redshift gives very high farinfrared luminosity – 1000 times that of our galaxy. Making basic assumptions about the source properties one gets estimates for the mass of dust of ~100 million solar masses. Assuming powered by star formati ...
... What do we know about these sources: Sub-mm flux combined with redshift gives very high farinfrared luminosity – 1000 times that of our galaxy. Making basic assumptions about the source properties one gets estimates for the mass of dust of ~100 million solar masses. Assuming powered by star formati ...
Slide 1
... collide and eventually form a single galaxy. • So much space between the stars that they ...
... collide and eventually form a single galaxy. • So much space between the stars that they ...
Megamaser
A megamaser is a type of astrophysical maser, which is a naturally occurring source of stimulated spectral line emission. Megamasers are distinguished from astrophysical masers by their large isotropic luminosity. Megamasers have typical luminosities of 103 solar luminosities (L☉), which is 100 million times brighter than masers in the Milky Way, hence the prefix mega. Likewise, the term kilomaser is used to describe masers outside the Milky Way that have luminosities of order L☉, or thousands of times stronger than the average maser in the Milky Way, gigamaser is used to describe masers billions of times stronger than the average maser in the Milky Way, and extragalactic maser encompasses all masers found outside the Milky Way. Most known extragalactic masers are megamasers, and the majority of megamasers are hydroxyl (OH) megamasers, meaning the spectral line being amplified is one due to a transition in the hydroxyl molecule. There are known megamasers for three other molecules: water (H2O), formaldehyde (H2CO), and methine (CH).Water megamasers were the first type of megamaser discovered. The first water megamaser was found in 1979 in NGC 4945, a galaxy in the nearby Centaurus A/M83 Group. The first hydroxyl megamaser was found in 1982 in Arp 220, which is the nearest ultraluminous infrared galaxy to the Milky Way. All subsequent OH megamasers that have been discovered are also in luminous infrared galaxies, and there are a small number of OH kilomasers hosted in galaxies with lower infrared luminosities. Most luminous infrared galaxies have recently merged or interacted with another galaxy, and are undergoing a burst of star formation. Many of the characteristics of the emission in hydroxyl megamasers are distinct from that of hydroxyl masers within the Milky Way, including the amplification of background radiation and the ratio of hydroxyl lines at different frequencies. The population inversion in hydroxyl molecules is produced by far infrared radiation that results from absorption and re-emission of light from forming stars by surrounding interstellar dust. Zeeman splitting of hydroxyl megamaser lines may be used to measure magnetic fields in the masing regions, and this application represents the first detection of Zeeman splitting in a galaxy other than the Milky Way.Water megamasers and kilomasers are found primarily associated with active galactic nuclei, while galactic and weaker extragalactic water masers are found in star forming regions. Despite different environments, the circumstances that produce extragalactic water masers do not seem to be very different from those that produce galactic water masers. Observations of water megamasers have been used to make accurate measurements of distances to galaxies in order to provide constraints on the Hubble constant.