499 research outputs found
Glanmor (J. Cuillandre). —Mouez an Aochou(La voix des Grèves). — Poésies bretonnes accompagnées de leur traduction française et de plusieurs mélodies populaires
No full textLoth J. Glanmor (J. Cuillandre). —Mouez an Aochou(La voix des Grèves). — Poésies bretonnes accompagnées de leur traduction française et de plusieurs mélodies populaires. In: Annales de Bretagne. Tome 19, numéro 4, 1903. pp. 637-639
Glanmor (J. Cuillandre). — Mouez an Aochou (La voix des Grèves). — Poésies bretonnes accompagnées de leur traduction française et de plusieurs mélodies populaires
No full textLoth J. Glanmor (J. Cuillandre). — Mouez an Aochou (La voix des Grèves). — Poésies bretonnes accompagnées de leur traduction française et de plusieurs mélodies populaires. In: Annales de Bretagne. Tome 19, numéro 4, 1903. pp. 637-639
A propos de la "Légende de la Mort"
No full textCuillandre Joseph. A propos de la "Légende de la Mort". In: Annales de Bretagne. Tome 35, numéro 4, 1921. pp. 627-650
The
No full textThe surface brightness distribution (SBD) function describes the
number density of galaxies as measured against their central
surface brightness. Because detecting galaxies with low central surface
brightnesses is both time-consuming and complicated, determining the
shape of this distribution function can be difficult.
In a recent paper Cross et al. suggested
a bell-shaped SBD disk-galaxy function which peaks near the canonical Freeman
value of 21.7 and then falls off significantly by 23.5 B mag arcsec-2.
This is in contradiction to previous studies which have typically
found flat (slope = 0) SBD functions out to 24–25 B mag arcsec-2
(the survey limits). Here we take advantage of a
recent surface-brightness limited survey by Andreon & Cuillandre which
reaches considerably fainter magnitudes than the Cross et al. sample
(MB reaches fainter than -12 for Andreon & Cuillandre while
the Cross et al. sample is limited to 16)
to re-evaluate both the SBD function as found by their data and the SBD
for a wide variety of galaxy surveys, including the Cross et al. data.
The result is a SBD function with a flat slope out through
the survey limits of 24.5 B mag arcsec-2, with high confidence limits
Automating the Synthetic Field Method:Application to Sextans A
No full textHolwerda, B W; Allen, R J; Van der Kruit, P C; ( Kapteyn Institute Groningen ) ( Space Telescope Science Institute, ) 29 Jan 2002 . - 4 p Abstract: We have automated the ``Synthetic Field Method'' developed by Gonzalez et al.(1998) and used it to measure the opacity of the ISM in the Local Group dwarf galaxy Sextans A by using the changes in counts of background galaxies seen through the foreground system. The Sextans A results are consistent with the observational relation found by Cuillandre et al. (2001) between dust opacity and HI column density in the outer parts of M31
Automating the Synthetic Field Method : Application to Sextans A
No full textHolwerda, B W; Allen, R J; Van der Kruit, P C;
( Kapteyn Institute Groningen ) ( Space Telescope Science Institute, )
29 Jan 2002 . - 4 p
Abstract: We have automated the ``Synthetic Field Method'' developed by Gonzalez et al.(1998) and used it to measure the opacity of the ISM in the Local Group dwarf galaxy Sextans A by using the changes in counts of background galaxies seen through the foreground system. The Sextans A results are consistent with the observational relation found by Cuillandre et al. (2001) between dust opacity and HI column density in the outer parts of M31.
Automating the Synthetic Field Method:Application to Sextans A
No full textHolwerda, B W; Allen, R J; Van der Kruit, P C; ( Kapteyn Institute Groningen ) ( Space Telescope Science Institute, ) 29 Jan 2002 . - 4 p Abstract: We have automated the ``Synthetic Field Method'' developed by Gonzalez et al.(1998) and used it to measure the opacity of the ISM in the Local Group dwarf galaxy Sextans A by using the changes in counts of background galaxies seen through the foreground system. The Sextans A results are consistent with the observational relation found by Cuillandre et al. (2001) between dust opacity and HI column density in the outer parts of M31
Mapping accretion and its variability in the young open cluster NGC 2264: A study based on u-band photometry
No full textContext. The accretion process has a central role in the formation of stars and planets. Aims. We aim at characterizing the accretion properties of several hundred members of the star-forming cluster NGC 2264 (3 Myr). Methods. We performed a deep ugri mapping as well as a simultaneous u-band+r-band monitoring of the star-forming region with CFHT/MegaCam in order to directly probe the accretion process onto the star from UV excess measurements. Photometric properties and stellar parameters are determined homogeneously for about 750 monitored young objects, spanning the mass range Σ0.1-2 M. About 40% of the sample are classical (accreting) T Tauri stars, based on various diagnostics (Hα, UV and IR excesses). The remaining non-accreting members define the (photospheric + chromospheric) reference UV emission level over which flux excess is detected and measured. Results. We revise the membership status of cluster members based on UV accretion signatures, and report a new population of 50 classical T Tauri star (CTTS) candidates. A large range of UV excess is measured for the CTTS population, varying from a few times 0.1 to ~3 mag. We convert these values to accretion luminosities and accretion rates, via a phenomenological description of the accretion shock emission. We thus obtain mass accretion rates ranging from a few 10-10 to ∼10-7 M/yr. Taking into account a mass-dependent detection threshold for weakly accreting objects, we find a >6σ correlation between mass accretion rate and stellar mass. A power-law fit, properly accounting for censored data (upper limits), yields acc M∗1.4±0.3. At any given stellar mass, we find a large spread of accretion rates, extending over about 2 orders of magnitude. The monitoring of the UV excess on a timescale of a couple of weeks indicates that its variability typically amounts to 0.5 dex, i.e., much smaller than the observed spread in accretion rates. We suggest that a non-negligible age spread across the star-forming region may effectively contribute to the observed spread in accretion rates at a given mass. In addition, different accretion mechanisms (like, e.g., short-lived accretion bursts vs. more stable funnel-flow accretion) may be associated to different acc regimes. Conclusions. A huge variety of accretion properties is observed for young stellar objects in the NGC 2264 cluster. While a definite correlation seems to hold between mass accretion rate and stellar mass over the mass range probed here, the origin of the large intrinsic spread observed in mass accretion rates at any given mass remains to be explored
Automating the Synthetic Field Method: Application to Sextans A
No full textHolwerda, B W; Allen, R J; Van der Kruit, P C; ( Kapteyn Institute Groningen ) ( Space Telescope Science Institute, ) 29 Jan 2002 . - 4 p Abstract: We have automated the ``Synthetic Field Method'' developed by Gonzalez et al.(1998) and used it to measure the opacity of the ISM in the Local Group dwarf galaxy Sextans A by using the changes in counts of background galaxies seen through the foreground system. The Sextans A results are consistent with the observational relation found by Cuillandre et al. (2001) between dust opacity and HI column density in the outer parts of M31
An Economic Analysis of Electron Accelerators and Cobalt-60 for Irradiating Food
No full textAverage costs per pound of irradiating food are similar for the electron accelerator and cobalt-60 irradiators analyzed in this study, but initial investment costs can vary by $1 million. Irradiation costs range from 0.5 to 7 cents per pound and decrease as annual volumes treated increase. Cobalt-60 is less expensive than electron beams for annual volumes below 50 million pounds. For radiation source requirements above the equivalent of 1 million curies of cobalt-60, electron beams are more economical.food irradiation, electron accelerators, cobalt-60, cost comparison, economies of size, Food Consumption/Nutrition/Food Safety,
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