24 research outputs found
The Mid-Infrared Spectrum of the Zodiacal and Exozodiacal Light
The zodiacal light is the dominant source of the mid-infrared sky brightness
seen from Earth, and exozodiacal light is the dominant emission from planetary
and debris systems around other stars. We observed the zodiacal light spectrum
with ISOCAM over 5-16 over a wide range of orientations relative to the Sun and
the ecliptic. We present theoretical models for a wide range of particle size
distributions and compositions. The observed temperature is as expected for
large (>10 um radius), low-albedo (< 0.08), rapidly-rotating, grey particles 1
AU from the Sun. In addition to the continuum, we detect a weak excess in the
9-11 um range, with an amplitude of 6% of the continuum. The shape of the
feature can be matched by a mixture of silicates: amorphous forsterite/olivine,
dirty crystalline olivine, and a hydrous silicate (montmorillonite). The
presence of hydrous silicate suggests the parent bodies of those particles were
formed in the inner solar nebula. Large particles dominate the size
distribution, but at least some small particles (radii ~1 um) are required to
produce the silicate emission feature. To compare the properties of zodiacal
dust to dust around other main sequence stars, we reanalyzed the exozodiacal
light spectrum for Beta Pic. The exozodiacal spectra are dominated by cold
dust, with emission peaking in the far-infrared, while the zodiacal spectrum
peaks around 20 um. The shape of the silicate feature from Beta Pic is nearly
identical to that derived from the ISO spectrum of 51 Oph; both exozodiacal
features are very different from that of the zodiacal light. The exozodiacal
features are roughly triangular, peaking at 10.3 um while the zodiacal feature
is more boxy.Comment: accepted to Icaru
Windows in the Milky Way
The objectives were twofold: (1) to study the IRAS emission levels in the vicinity of Baade's Window and in other optically transparent regions near the Galactic Center; and (2) to study the IRAS emission levels along sightlines in the Milky Way that exhibit very little CO emission. Tests were attempted to see whether the optically transparent 'windows' near the Galactic center can be identified (as FIR-weak regions) in the IRAS data base; and if so, whether the CO weak regions found elsewhere in the Milky Way represent similarly FIR weak and thus optically transparent sightlines through the Galaxy. The CO weak regions were also targeted in an effort to study the diffuse intercloud dust and its warming by the interstellar radiation field
Operations and Performance of the PACS Instrument 3He Sorption Cooler on board of the Herschel Space Observatory
A 3He sorption cooler produced the operational temperature of 285mK for the
bolometer arrays of the Photodetector Array Camera and Spectrometer (PACS)
instrument of the Herschel Space Observatory. This cooler provided a stable
hold time between 60 and 73h, depending on the operational conditions of the
instrument. The respective hold time could be determined by a simple functional
relation established early on in the mission and reliably applied by the
scientific mission planning for the entire mission. After exhaustion of the
liquid 3He due to the heat input by the detector arrays, the cooler was
recycled for the next operational period following a well established automatic
procedure. We give an overview of the cooler operations and performance over
the entire mission and distinguishing in-between the start conditions for the
cooler recycling and the two main modes of PACS photometer operations. As a
spin-off, the cooler recycling temperature effects on the Herschel cryostat 4He
bath were utilized as an alternative method to dedicated Direct Liquid Helium
Content Measurements in determining the lifetime of the liquid Helium coolant.Comment: 34 pages, 13 figures, accepted in Experimental Astronom
Impacts of The Radiation Environment At L2 On Bolometers Onboard The Herschel Space Observatory
We present the effects of cosmic rays on the detectors onboard the Herschel
satellite. We describe in particular the glitches observed on the two types of
cryogenic far- infrared bolometer inside the two instruments PACS and SPIRE.
The glitch rates are also reported since the launch together with the SREM
radiation monitors aboard Herschel and Planck spacecrafts. Both have been
injected around the Lagrangian point L2 on May 2009. This allows probing the
radiation environment around this orbit. The impacts on the observation are
finally summarized.Comment: 8 pages, 13 figures, 2 images, Author Keywords: Bolometers, Infrared
detectors, cryogenics, radiation effects, submillimeter wave technology IEEE
Terms: Bolometers, Detectors, Instruments, Picture archiving and
communication systems, Protons, Silicon, Space vehicles; Radiation and Its
Effects on Components and Systems (RADECS), 2011 12th European Conference.
Conference location: Sevilla. Date of Conference: 19-23 Sept. 2011. Session
H: Radiation Environment: Space, Atmospheric and Terrestrial (PH2
The Herschel PACS photometer calibration - A time dependent flux calibration for the PACS chopped point-source photometry AOT mode
We present a flux calibration scheme for the PACS chopped point-source
photometry observing mode based on the photometry of five stellar standard
sources. This mode was used for science observations only early in the mission.
Later, it was only used for pointing and flux calibration measurements. Its
calibration turns this type of observation into fully validated data products
in the Herschel Science Archive. Systematic differences in calibration with
regard to the principal photometer observation mode, the scan map, are derived
and amount to 5-6%. An empirical method to calibrate out an apparent response
drift during the first 300 Operational Days is presented. The relative
photometric calibration accuracy (repeatability) is as good as 1% in the blue
and green band and up to 5% in the red band. Like for the scan map mode,
inconsistencies among the stellar calibration models become visible and amount
to 2% for the five standard stars used. The absolute calibration accuracy is
therefore mainly limited by the model uncertainty, which is 5% for all three
bands.Comment: 20 pages, 7 pages of appendix, 11 figures, accepted to appear in
Experimental Astronomy, Special Issue for Herschel Calibrations based on the
"Herschel Calibration Workshop: Only the Best Data Products for the Legacy
Archive", held at ESAC, 25 - 27 March 2013,
http://herschel.esac.esa.int/CalibrationWorkshop5.shtm
The Spatial Distribution of Dust and Stellar Emission of the Magellanic Clouds
We study the emission by dust and stars in the Large and Small Magellanic
Clouds, a pair of low-metallicity nearby galaxies, as traced by their spatially
resolved spectral energy distributions (SEDs). This project combines Herschel
Space Observatory PACS and SPIRE far-infrared photometry with other data at
infrared and optical wavelengths. We build maps of dust and stellar luminosity
and mass of both Magellanic Clouds, and analyze the spatial distribution of
dust/stellar luminosity and mass ratios. These ratios vary considerably
throughout the galaxies, generally between the range and .
We observe that the dust/stellar ratios depend on the interstellar medium (ISM)
environment, such as the distance from currently or previously star-forming
regions, and on the intensity of the interstellar radiation field (ISRF). In
addition, we construct star formation rate (SFR) maps, and find that the SFR is
correlated with the dust/stellar luminosity and dust temperature in both
galaxies, demonstrating the relation between star formation, dust emission and
heating, though these correlations exhibit substantial scatter.Comment: 15 pages, 18 figures; ApJ, in press; version published in the journal
will have higher-resolution figure
Localized Surface Plasmon Resonance of Metallic Nanoparticles--Optical Property Characterization for Rational Applications
在光的激发下金属纳米结构中的自由电子能够发生群体性的振荡,进而产生表面等离激元(SPP)。发生等离激元共振时,金属纳米结构会将光束缚在表面,并在表面产生极强的电场增强。表面等离激元有两种类型:一类具有传播的特点,其表面等离激元能够在表面传播,称之为propagatingSPP;另一类不具有传播性,共振局域在一个很小的金属结构中,称之为localizedSPP,即局域表面等离激元共振(LSPR)。金属纳米颗粒就具有很强的表面等离激元共振的(LSPR)性质,使其对光产生增强的吸收和增强的散射,并表现出相关的热、光电场增强和热电子等效应。近年,随着纳米科技的发展,金属纳米粒子的LSPR效应已经成为一...The collective oscillation of free electrons in metal nanostructures excited with light is called surface plasmon polaritons (SPP). The light will be confined to a small area on the surface under the resonance condition (SPR), thus a giant enhancement in the electric field will be produced. There are two kinds of surface plasmon polaritons (SPP): one is propagating plasmon polaritons (PSPP), which...学位:理学博士院系专业:化学化工学院_物理化学(含化学物理)学号:2052010015366