A Digital Spectral Classification Atlas
... The MK Spectral classification system was founded by W.W. Morgan and P.C. Keenan in the year 1943, with the publication of the first photographic spectral classification atlas, An Atlas of Stellar Spectra (Morgan, Keenan & Kelleman, 1943). Since that time, the MK system has been extensively revised ...
... The MK Spectral classification system was founded by W.W. Morgan and P.C. Keenan in the year 1943, with the publication of the first photographic spectral classification atlas, An Atlas of Stellar Spectra (Morgan, Keenan & Kelleman, 1943). Since that time, the MK system has been extensively revised ...
April 2015 Astronomy Calendar by Dave Mitsky
... Mercury, Venus, and Mars are located in the west and Jupiter in the south in the evening. At midnight, Jupiter is in the west, and Saturn is in the southeast. Saturn can be found in the southwest and Uranus and Neptune in the east in the morning sky. At midmonth, Venus sets at 11:00 p.m., Mars sets ...
... Mercury, Venus, and Mars are located in the west and Jupiter in the south in the evening. At midnight, Jupiter is in the west, and Saturn is in the southeast. Saturn can be found in the southwest and Uranus and Neptune in the east in the morning sky. At midmonth, Venus sets at 11:00 p.m., Mars sets ...
IRAM Annual Report 2012
... maintain its know-how and leading position in mmwave instrumentation. At the time when this report is edited, another important change at IRAM has taken place. After more than 8 years of duty as the IRAM director, Pierre Cox has started his new position as the director of ALMA in Santiago, Chile. I ...
... maintain its know-how and leading position in mmwave instrumentation. At the time when this report is edited, another important change at IRAM has taken place. After more than 8 years of duty as the IRAM director, Pierre Cox has started his new position as the director of ALMA in Santiago, Chile. I ...
from z=0 to z=1
... IR/UV increases by ~ 4. This is consistent with the scenario that high z galaxies are more luminous therefore with higher attenuation. ...
... IR/UV increases by ~ 4. This is consistent with the scenario that high z galaxies are more luminous therefore with higher attenuation. ...
Star Formation in the Milky Way and Nearby Galaxies Further
... between the community studying individual star-forming regions and stars in the Milky Way (MW; also sometimes referred to as the Galaxy) and the largely extragalactic community that attempts to characterize the star-formation process on galactic and cosmological scales. Some aspects of this separati ...
... between the community studying individual star-forming regions and stars in the Milky Way (MW; also sometimes referred to as the Galaxy) and the largely extragalactic community that attempts to characterize the star-formation process on galactic and cosmological scales. Some aspects of this separati ...
1 Globular Cluster Systems - McMaster Physics and Astronomy
... these heavily reddened clusters remained surprisingly poor, and even today there are still a few clusters with exceptionally high reddenings embedded deep in the Galactic bulge about which we know almost nothing (see the listings in Harris 1996a). However, progress over the years has been steady and ...
... these heavily reddened clusters remained surprisingly poor, and even today there are still a few clusters with exceptionally high reddenings embedded deep in the Galactic bulge about which we know almost nothing (see the listings in Harris 1996a). However, progress over the years has been steady and ...
Physical Properties of the Gas and Dust in the Orion B Molecular
... are located (see Goudis 1982 for a review). Their strong UV radiation field and stellar winds impinge on the “surface” of the molecular cloud form this side. The main internal heating source of L 1630 is the H II region NGC 2024 which is the second most luminous source in the Orion region and the on ...
... are located (see Goudis 1982 for a review). Their strong UV radiation field and stellar winds impinge on the “surface” of the molecular cloud form this side. The main internal heating source of L 1630 is the H II region NGC 2024 which is the second most luminous source in the Orion region and the on ...
Luminosity profiles and sizes of massive star clusters in NGC 7252
... radii Reff of 36 young massive clusters (YMCs) within the galaxy. All the clusters have masses exceeding 105 M and are, despite the 64 Mpc distance to the galaxy, (partly) resolved on the HST images. Effective radii can be measured down to ∼2.5 pc, and the largest clusters have Reff approaching 20 ...
... radii Reff of 36 young massive clusters (YMCs) within the galaxy. All the clusters have masses exceeding 105 M and are, despite the 64 Mpc distance to the galaxy, (partly) resolved on the HST images. Effective radii can be measured down to ∼2.5 pc, and the largest clusters have Reff approaching 20 ...
1998 - Universitäts-Sternwarte München
... found to be metal-poor objects – as opposed to the understanding when they were first analyzed in the 1950s. Interestingly, these stars also reveal a very different kinematic behaviour in that they do not take share in the rotation of the Galactic disk, i.e. they constitute a different stellar popul ...
... found to be metal-poor objects – as opposed to the understanding when they were first analyzed in the 1950s. Interestingly, these stars also reveal a very different kinematic behaviour in that they do not take share in the rotation of the Galactic disk, i.e. they constitute a different stellar popul ...
Galactic Stellar and Substellar Initial Mass Function Invited Review Gilles Chabrier
... kinematic shear between the thick-disk population, present in local samples, and the genuine spheroid one. This enables us to derive only an upper limit for the spheroid mass density and IMF. Within all the uncertainties, the latter is found to be similar to the one derived for globular clusters and ...
... kinematic shear between the thick-disk population, present in local samples, and the genuine spheroid one. This enables us to derive only an upper limit for the spheroid mass density and IMF. Within all the uncertainties, the latter is found to be similar to the one derived for globular clusters and ...
An Expanded View of the Universe
... the Universe? Black holes have puzzled physicists and astronomers since they were first postulated in relativistic form a century ago by Karl Schwarzschild. Observations have demonstrated that these bizarre objects really exist. And on a grand scale, too: not only have black holes been found with ma ...
... the Universe? Black holes have puzzled physicists and astronomers since they were first postulated in relativistic form a century ago by Karl Schwarzschild. Observations have demonstrated that these bizarre objects really exist. And on a grand scale, too: not only have black holes been found with ma ...
IRAM Annual Report 2014
... One of the challenges in understanding how stars form is how massive clouds of gas and dust fragment to produce the direct progenitors of individual stars. In order to shed new light on the formation of stars more than 10 times the mass of our Sun, an international team of astronomers led by Nicolas ...
... One of the challenges in understanding how stars form is how massive clouds of gas and dust fragment to produce the direct progenitors of individual stars. In order to shed new light on the formation of stars more than 10 times the mass of our Sun, an international team of astronomers led by Nicolas ...
Jul y 10-12,
... center with Chandra, following up XRTs with HST; 4σ B magnitude limits for counterparts are ∼ 26 − 29. We obtain period estimates for each XRT for both neutron star and BH accretors. These M31 XRTs appear to be somewhat skewed towards shorter periods than XRTs in the Milky Way. ...
... center with Chandra, following up XRTs with HST; 4σ B magnitude limits for counterparts are ∼ 26 − 29. We obtain period estimates for each XRT for both neutron star and BH accretors. These M31 XRTs appear to be somewhat skewed towards shorter periods than XRTs in the Milky Way. ...
Probing nuclear activity versus star formation at z ∼ 0.8 using near
... starburst, AGN and galaxy templates from Polletta et al. (2007). Based on this SED fitting, we classified them as AGN-dominated (52 per cent) and host galaxy-dominated (48 per cent) objects. The latter have SEDs typical of starburst, spiral or elliptical galaxies, indicating the presence of a deeply ...
... starburst, AGN and galaxy templates from Polletta et al. (2007). Based on this SED fitting, we classified them as AGN-dominated (52 per cent) and host galaxy-dominated (48 per cent) objects. The latter have SEDs typical of starburst, spiral or elliptical galaxies, indicating the presence of a deeply ...
probing quasar environments with tunable filter
... AGN may be categorised in a variety of ways; a simple taxonomy is shown in table 1.1, in which they are classified according to two parameters: radio-loudness and the width of their emission lines. Sometimes, more than one class of object shares a given radio categorisation and optical type: these a ...
... AGN may be categorised in a variety of ways; a simple taxonomy is shown in table 1.1, in which they are classified according to two parameters: radio-loudness and the width of their emission lines. Sometimes, more than one class of object shares a given radio categorisation and optical type: these a ...
Galaxies - hwchemistry
... and used the Hubble Space Telescope to record a time exposure that lasted an astonishing 10 days. – This became known as a Hubble deep field. – It was deep in that it recorded very faint objects. – The image revealed that the ‘empty spot’ on the sky was filled with galaxies. ...
... and used the Hubble Space Telescope to record a time exposure that lasted an astonishing 10 days. – This became known as a Hubble deep field. – It was deep in that it recorded very faint objects. – The image revealed that the ‘empty spot’ on the sky was filled with galaxies. ...
2 Justification and benefits in joining TMT
... advanced adaptive optics will revolutionise many fields in astronomy. TMT will directly image and probe the atmospheres of extrasolar planets; it will provide key insights into the nature of dark matter and dark energy, and shed light on how galaxies, stars, black holes and planets form and evolve. ...
... advanced adaptive optics will revolutionise many fields in astronomy. TMT will directly image and probe the atmospheres of extrasolar planets; it will provide key insights into the nature of dark matter and dark energy, and shed light on how galaxies, stars, black holes and planets form and evolve. ...
DUSTiNGS III: Distribution of Intermediate
... et al. 2007; Vijh et al. 2009), thereby eliminating confusion with other infrared-bright point sources. In total, DUSTiNGS identified 710 variable AGB star candidates including 526 variable x-AGB star candidates (Boyer et al. 2015c, hereafter Paper II). Twelve of these x-AGB star candidates are in g ...
... et al. 2007; Vijh et al. 2009), thereby eliminating confusion with other infrared-bright point sources. In total, DUSTiNGS identified 710 variable AGB star candidates including 526 variable x-AGB star candidates (Boyer et al. 2015c, hereafter Paper II). Twelve of these x-AGB star candidates are in g ...
WILLIAM HERSCHEL AND THE `GARNET` STARS: μ CEPHEI AND
... at often. Very beautiful indeed. (Herschel, W., 1782a: 32; see Figure 3). ...
... at often. Very beautiful indeed. (Herschel, W., 1782a: 32; see Figure 3). ...
Far-ultraviolet and far-infrared bivariate luminosity function of galaxies:
... because they were not based on a well-controlled sample of FUV and FIR selected galaxies. Recently, thanks to new large surveys, some attempts to explore the SFR distribution of galaxies in a bivariate way have been made, through the “SFR function” (e.g., Buat et al., 2007, 2009; Bothwell et al., 20 ...
... because they were not based on a well-controlled sample of FUV and FIR selected galaxies. Recently, thanks to new large surveys, some attempts to explore the SFR distribution of galaxies in a bivariate way have been made, through the “SFR function” (e.g., Buat et al., 2007, 2009; Bothwell et al., 20 ...
Annual Report 2011 - Max Planck Institute for Astrophysics
... cated the MPA to its current site. The MPA becomputational capabilities are expected to lead came fully independent in 1991. Kippenhahn reto rapid developments. Active areas of current tired shortly thereafter and this led to a period of research include stellar evolution, stellar atmouncertainty, w ...
... cated the MPA to its current site. The MPA becomputational capabilities are expected to lead came fully independent in 1991. Kippenhahn reto rapid developments. Active areas of current tired shortly thereafter and this led to a period of research include stellar evolution, stellar atmouncertainty, w ...
Markov Chain Monte Carlo Modeling of High-Redshift Quasar
... and ν is the frequency. The power-law spectrum was punctuated by extremely broad emission lines (equivalent widths of '50 Å), indicating emission from ionized gas with extremely high velocities ('10,000 km s−1 ). Schmidt identified emission lines as the Balmer series of Hydrogen, with a systematic ...
... and ν is the frequency. The power-law spectrum was punctuated by extremely broad emission lines (equivalent widths of '50 Å), indicating emission from ionized gas with extremely high velocities ('10,000 km s−1 ). Schmidt identified emission lines as the Balmer series of Hydrogen, with a systematic ...
Science Case for the Chinese Participation of TMT
... advanced adaptive optics will revolutionise many fields in astronomy. TMT will directly image and probe the atmospheres of extrasolar planets; it will provide key insights into the nature of dark matter and dark energy, and shed light on how galaxies, stars, black holes and planets form and evolve. ...
... advanced adaptive optics will revolutionise many fields in astronomy. TMT will directly image and probe the atmospheres of extrasolar planets; it will provide key insights into the nature of dark matter and dark energy, and shed light on how galaxies, stars, black holes and planets form and evolve. ...
JENAM-2011 Book of abstracts
... The X-ray appearance of majority of normal galaxies is determined by radiation from accreting neutron stars and stellar mass black holes in X-ray binaries. Chandra and XMM-Newton observations revealed that their populations scale with the star-formation rate and stellar mass of the host galaxy. Thus ...
... The X-ray appearance of majority of normal galaxies is determined by radiation from accreting neutron stars and stellar mass black holes in X-ray binaries. Chandra and XMM-Newton observations revealed that their populations scale with the star-formation rate and stellar mass of the host galaxy. Thus ...
N-Body/SPH simulations of induced star formation in dwarf galaxies
... increased and will attract other clumps. These clumps will start moving, attracting one another, and merge. When the formed structures of dark matter and baryons contain a sufficient amount of baryonic gas, they can start forming stars and dwarf galaxies are born. Large galaxies as for instance our ...
... increased and will attract other clumps. These clumps will start moving, attracting one another, and merge. When the formed structures of dark matter and baryons contain a sufficient amount of baryonic gas, they can start forming stars and dwarf galaxies are born. Large galaxies as for instance our ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.