hi-fi
NHSC HIFI - The Heterodyne Instrument for the Far Infrared
+ Home Page
+ Search NASA Herschel Site
+ NASA Herschel Science Center
- Observation Planning
*
FAQs
*
HSpot (planning tool)
*
AOR planning
*
Reserved Observation List
*
Proposal Calls
*
Past Proposal Calls
- Workshops
- Proposal Information
*
Approved Programs
- Newsletters
- Logos
+ Herschel Mission
+ Herschel Instruments
+
JPL Herschel Page
+ NHSC Staff
+ Speaker's Bureau
+
Cool Cosmos (Education)
+ Helpdesk
+ Contact Us
ESA Links
Herschel Science Center
(HSC-ESAC-Spain)
+ Main HSC Home Page
+ HSC Community Information
+ HSC Science Instruments Page
+ HSC AO Documentation
+ HSC AO Latest News
+ HSC European Helpdesk
+ Images & Videos
+
Herschel/ALMA Synergies
+
IPAC Homepage
+
IPAC Newsletter
+
IPAC Visiting Graduate Student Fellowship Program
+
IPAC Visitor Information
+ Additional Links
HIFI
The
Heterodyne
Instrument
for the Far Infrared
A very
high resolution spectrometer covering 480 - 1910 GHz (625 - 157
µm)
Introduction
HIFI
Quick Facts
NHSC
HIFI Support
Rendition of the HIFI Focal Plane
Unit (FPU)
The HIFI FPU
Qualifcation
Module prepared for cold vibration tests,
CSL (Liège), Summer 2005.
Introduction
Click
here for
a pdf "Pocket Guide" to HIFI - a flyer we have prepared and
keep updated for venues such as meetings of the AAS.
Why HIFI The
HIFI instrument is designed to allow observations of astrophysically
important molecular and atomic transitions occuring in the
far-infrared, at ultra-high
frequency resolutions and sensitivities not possible at existing
ground-based facilities. Data from
HIFI will produce very detailed spectra revealing the motions,
temperatures, and other characteristics of the atoms and molecules
accessible to HIFI's receiving devices. This in turn will help
scientists understand the processes that govern comets, planetary
atmospheres, star formation, and the development of distant and nearby
galaxies.
Novel
Technology HIFI is more than just heterodyne receivers
launched into orbit in order to overcome the low
transmission
of radiation through the Earth's atmosphere at critical wavelengths
(due mainly to water). The far-infrared/submillimeter range falls in between
the high performance regimes of transistors (used for microwave
observations) and Si or Ge blocked impurity band (BiB) detectors (used
in the mid-infrared). HIFI's receivers represent hybrids between
conventional and quantum electronics that push the limits of
technology, employing a combination of
superconductor-insulator-superconductor (SIS) and hot electron
bolometer (HEB) mixing devices in the HIFI receivers to detect weak
signals with very little noise (goal 3 h×nu/k).
NASA-funded work at JPL on the mixing elements for the
highest-frequency bands, as well as the frequency sources for these
bands and components of the sources for the remaining bands, are
cruicial parts of these record-setting innovations, described at JPL's public
HIFI technology page.
Back to
the
top
HIFI Quick Facts
Principal Investigator: Thijs
de Graauw, Netherlands Institute for
Space Research
Co-Principal Investigators:
Tom Phillips, Caltech
Emmanual Caux, CESR
Jьrgen Stutzki, Univ.
Kцln
Science Drivers: Visit the HIFI Science Page at
SRON.
Instrument Control Center: HIFI-ICC -
operational nerve center and Project Office site at the PI institute in
Groningen, NL
Properties and Expected
Sensitivities:
Mixer Band1
Element
1
SIS3
2
SIS4
3
SIS4
4
SIS4
5
SIS5
6L,6H2
HEB6
Frequency Coverage [GHz]
480-640
640-800
800-960
960-1120
1120-1250
1410-1910
Beam
Sizes (Half Power Beam Width, averaged) [arcsec]
41
29
25
21
18.5
14.5,
12.5
Receiver Noise (DSB7, Baseline/Goal) [K]
90/84
130/120
170/160
210/190
370/210
650/650
Flux Limit (5-sig, 1hr, R=104)
[Jy/mK]
1.5/3.4
2.0/4.4
2.3/5.1
2.5/5.6
2.7/6.0
4.6/10
Line Flux Limit (5-sig, 1hr, R=104) [10-18
W m-2]
0.9
1.4
2.0
2.6
3.2
7.0
Line Scan (1-sig, 24hr, f=1MHz) [mK]
16
16
16
16
16
34
1 Two mixers per band provide
dual (H and V) polarization.
2 Band 6 is
divided into Low (1410-1703 GHz) and High (1703-1910 GHz) regimes, each
employing separate mixer assemblies and local oscillator chains.
3 Nb-Al2O3-Nb
4
NbTiN-Al2O3-Nb
5
NbTiN-AlN-NbTi
6 NbN
phonon cooled
7 Dual Side
Band convolved.
Spectrometers and Resolutions:
Wide Band Spectrometer
Acousto-Optical Spectrometer
4 x 4 GHz sections
1 MHz (0.6 km s-1 @ 480
GHz)
High Resolution Spectrometer
Digital Auto-Correlator
2, 4 or 8 x 250 MHz sections (max
2 GHz
bandwidth) - 550 MHz samplers
0.14, 0.28, 0.56, 1.0 (wide band
mode) MHz
Radiometric Calibration Uncertainty: 10% baseline, 3% goal.
Hardware Fabrication: 22 institutes in 11 countries
NASA-funded hardware: NASA
is providing the mixers and local oscillator chains for the two highest
bands, 5 and 6 (where 6 is actually divided into two phonon-cooled
HEB bands), as well as other local oscillator components for bands 1
through 4, and power amplifiers. Work has been conducted
at JPL.
Observing Modes:
Single
Target, On-the-Fly
Mapping, and Spectral Scan Astronomical Observing Templates
(AOTs),
calibrated in modes employing position switching, dual beam switching,
frequency
throwing, and thermal load chopping. An observer's
manual will be made available by the Herschel Science Center (HSC);
important information on the observing mode defintions, applications,
and
restrictions is found in the HIFI Observing Modes Description
Document, written
for HIFI team members and users.
Observation Planning and
Proposal Submission Tools: available in Herschel-SPOT
(HSPOT), adapted from the Spitzer Planning and Observation Tool by
arrangement between the NHSC, the Spitzer Science Center, and the HSC.
Data Access and Processing: The Herschel data archive will be
hosted
at ESA's European Space Astronomy Centre (formerly Vilspa) in
Villafranca
del Castillo, Spain. Users of the ISO, XMM, and IUE archives will
be
familiar with this location. Unlike the ISO data processing
piplines,
however, which were based variously on fortran, IDL, and C, the
Herschel
Standard Product Generation software is being implemented in java,
based
on development in the interactive Data Processing (DP) environment of
the
exportable Herschel Common Software System (HCSS). Data
processing
in the HCSS is also rooted in the object-oriented java language,
with
Jython scripting cabilities in the user interface. The HIFI
interactive
DP environment is part of the HCSS, and is being used during pre-launch
instrument
tests and then during operations by calibration scientists. The
HCSS
and its instrument DP environments will be available to users.
Back to
the
top
HIFI Support at the NHSC
Our Tasks The
NHSC has a growing group of scientists and developers dedicated to
supporting US
astronomers who anticipate making use of HIFI in guaranteed and open
time science programs. However, we are not (or not only)
an observer support group for information relay. Effecitve
support comes from participating in the pre-launch preparations,
check-out, and routine maintenance activities in calibration scientist
and software developer roles, in agreement with and
coordination by the HIFI ICC "primary node". This includes as
many phases
as our staff can manage with time and travel, particpating in uplink
development
(observing modes, observation planning software), basic data
processing,
scientific analysis software development, instrument testing and
performance
verification. Since our scientists also anticipate using HIFI in
Guaranteed
and Open Time Key Programs, they can be relied upon to provide the
highest
quality support in program preparation, observation planning, and
data
access, processing and management, with specific attention to
needs of
the US astronomical community.
In addition to NHSC's
helpdesk system, these pages will provide HIFI-related information
about observation planning and data processing workshops, a frequenly
asked questions page, a wiki-based web collaboration between HIFI users
(according to need and interest),
and pathways to additional documentation and scientific resources.
These
will appear in time leading up to the Announcement of Opportunity for
Open
Time Key Programs.
Who We Are
Steve Lord -
Liaison Scientist
Pat Morris
- Liaison Scientist, group
lead
Joan Xie -
Software Engineer
30+ years combined experience with
the building, testing, operation, and calibration of instruments built
and shot into space on observatories for doing science, including ESA's
Infrared Space Observatory
and NASA's Spitzer Space
Telescope.
We also receive valuable
assistance and
guidance in system architecture and infrastructure from John Rector and
Jonathan
Kakumasu.
Back to
the
top
разделы
обзвон
конвейер
купить каболка
профессиональный видеосъемка
прерывание беременность
нард скачать бесплатный
touch screen
арочный конструкция
фирменый цвет
купить ниппель перех
метрореклама нижнийновгород
восстановление файл
измеритель освещенность
электрический прочность
управление архангельск
профессиональный видеосъемка
тонировка стекол
nokia 6021 купить
пломбирование
врач акушер гинеколог
штамповка
sharp ar-5415
креатин
терапевтический гидромассаж
футбольный тотализатор
купить айсбест
телематические служба
измеритель освещенность
renu multiplus 355мл
добрый тепло
ливнесборные решетка
очки ночной видение
сервер hp
фирменный флаг
кс-4361
красный площадь васильевский спуск
заказать обед
фосфоресцирующий краска
вскрытие авто
бюро похоронный услуга
hi-fi