Knowledgebase
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General(23)
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Finderchart(5)
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Spitzer(181)
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WISE(12)
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Planck(8)
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2MASS(5)
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IRAS(5)
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Herschel(1)
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Catalog Search(18)
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Table Upload(12)
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VO/API(1)
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WISE All-Sky Data Release Documentation [1]
WISE 3-Band Cryo Data Release Documentation [2]
NEOWISE Post-Cryo Preliminary Release Documentation [3]
More WISE Resources [4]
Links:
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[1] http://wise2.ipac.caltech.edu/docs/release/allsky
[2] h...
2MASS Documentation [1]
More 2MASS Resources [2]
Links:
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[1] http://www.ipac.caltech.edu/2mass/
[2] http://irsa.ipac.caltech.edu/Missions/2mass.html
IRAS Documentation [1]
More IRAS Resources [2]
Links:
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[1] http://irsa.ipac.caltech.edu/IRASdocs/iras.html
[2] http://irsa.ipac.caltech.edu/Missions/iras.html
Planck Data Release 1 Documentation (pdf) [1]
Planck Data Release 1 Documentation (ESA wiki) [2]
The PDF version misses some figures and references compared to the
wiki.
NASA Planck Archive Known Bugs and Issues [3]
More Planck resources [4...
SHA Known Bugs and Issues [1]
Links:
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[1] http://irsa.ipac.caltech.edu/docs/known_issues/shabugslist.html
Quick Guide [1]
Tutorial [2]
Program Interface Guide [3]
Links:
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[1]
http://irsa.ipac.caltech.edu/applications/Gator/GatorAid/irsa/QuickGuidetoGator.htm
[2]
http://irsa.ipac.caltech.edu/applications/Gator/GatorAid/irsa/Tutorial/tutorial.htm
[3...
The error message:
Perl system() return code = 6
sourcestimate ran with signal 6
System Exit Code ( sourcestimate): 6
usually means that you an out of RAM because of big blends of
detections in the detection table. The module Source Estimate perfor...
The answer can be found in this file [1].
Links:
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[1] http://ssc.spitzer.caltech.edu/faqs/spitzerorbit.txt
To understand where the IRAC zmag comes from, you can start with the
fundamental equation between magnitudes and flux densities. In one
incarnation, it becomes
m - M0 = -2.5*log(F/F0)
Here m is the magnitude of the source you want to measure, M0 is ...
IRAC images are in units of MJy/sr. If you want to convert them into
flux density/pixel units, you can convert steradians into arcsecconds
squared, and then multiply by the area of the pixel. Remember that in
BCDs the pixel area is approximately 1.22 arcs...
Here are some common definitions. The archive of Spitzer data is the
Spitzer Heritage Archive (SHA). An individual Spitzer observation
sequence is an AOR, or Astronomical Observation Request. In certain
cases (often calibration or sometimes science observ...
The columns that are returned are exactly those that are stored in the
archive for that catalog. Each catalog is different. Please check the
project's documentation for each catalog separately, all of which are
available at IRSA. Some of the more commonly...
The following page describes the basic IPAC Table Format, which can
be used with IRSA Services that support multi-object searches.
http://irsa.ipac.caltech.edu/applications/DDGEN/Doc/ipac_tbl.html
Please pay particular attention to the "DBMS Cons...
Depending on the nature of the constraints, you could be looking at
downloading a very large number of objects. To prevent a single user's
very large query from impacting our performance for other users,
IRSA's catalog search tool will fail for queries...
For Mac versions starting with Lion and some settings of Gatekeeper,
you may receive the following error message when you attempt to run
Mopex:
"Mopex" is damaged and can't be opened. You should move it to the
Trash.
Click "Cancel". You will need t...
While both the intensity and covariance quantities presented in the
Planck all-sky maps are, by definition, positive, there are situations
in which you will see negative values.
o In regards to the Planck intensity maps:
To begin with, the Planck...
The Planck map products express intensity in three different (and
frequency-dependent) forms: K_CMB (thermodynamic temperature), K_RJ
(antenna temperature, also know as Rayleigh-Jeans temperature), and
MJy/sr. The attached memo addresses the definition...
You cannot input a list of object names directly into the Catalog
Search Tool. However, you can feed your list (with no header) into the
IPAC Table Reformat and Validation Service:
http://irsa.ipac.caltech.edu/applications/TblCheck/ [1]
If you cl...
The standard IRSA acknowledgment [1] is:
This research has made use of the NASA/ IPAC Infrared Science
Archive, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National
Aeronautics and Space...
QUICK START GUIDE TO USING THE SPITZER ENHANCED IMAGING PRODUCTS
Let's assume you are using standalone tools to access the Spitzer
Enhanced Imaging Products (that is, working outside the Spitzer
Heritage Archive). You can get the Super Mosaics coverin...
Yes, but it has to be in the same format as the Spitzer ASCII tables
before you can do that. The only exception is 2MASS data, which can be
read directly by Bandmerge if you set the project flag to 2 (1 is the
default and applies to Spitzer data). For exa...
As part of the closeout for the Spitzer cryogenic mission custody of
Spitzer documentation was transferred from the Spitzer Science Center
to the Infrared Science Archive (IRSA) in April of 2011. However some
information needed to run the warm mission was...
The chances are that it's neither of the above. Most likely the
overall gradient in the mosaic image comes from the gradients in the
input images, which were not properly flat-fielded. This is sometimes
seen in MIPS-24 images. Perl script flatfield.pl, in...
Check the uncertainty images - they could be overestimated.
There are no restrictions on the mosaic pixel size. If the mosaic
pixel size is so small that you don't have enough computer memory to
coadd all the interpolated images at once, you should split the mosaic
into several tiles. In order to do so, a suggeste...
The projection used here is exact, it involves no approximations. The
only requirement here is that the final mosaic can not span more than
one hemisphere.
Yes. First you should produce a mosaic with the corresponding
uncertainty image. Then you run apex_1frame.pl (APEX Single Frame in
the GUI) setting INPUT_IMAGE_FILE = and SIGMA_IMAGE_FILE = . Use the
appropriate PRF file. PRF fitting is not recommended o...
There are 4 interpolation methods available in MOPEX: DEFAULT (1),
DRIZZLE (2), GRID (3), and CUBIC (4).
GRID should be used when a quick-look mosaic is needed. It can also
be used for background matching (overlap.pl). The gain in speed is up
to 10 time...
This is possible with the APEX "User List" flows. See the MOPEX User's
Guide [1] for more information.
Links:
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[1]
http://ssc.spitzer.caltech.edu/dataanalysistools/tools/mopex/mopexusersguide/
The command-line version of MOPEX is distributed with the GUI - you
should download the GUI and follow the installation instructions on
the MOPEX Download page [1]. Note that the environment variable file
for MOPEX has changed from mopex.csh in previous v...
Here is an example FIF.tbl file, which is by default placed in your
output directory by the MOPEX module Fiducial Image Frame.
********************************************************************************
\char comment = Output from fiducial_image_f...
The pixel size can be set directly using the following keywords in the
namelist, or in the Initial Settings module > General Options in the
GUI:
MOSAIC_PIXEL_SIZE_X = -0.0003
MOSAIC_PIXEL_SIZE_Y = 0.0003
MOSAIC_PIXEL_SIZE_X is negative to follow the ...
The slowest step is image interpolation. On a 500 MHz Sunblade with
512 MB of memory, it takes ~20s to process a 256x256 image.
The way to avoid doing passive deblending is to remove the
deblend_size and deblend_id columns. To do so on the command line, set
the following in the namelist:
run_select_detect = 1
and add the list of columns to copy:
select_detect_columns = "srcid...
1) Run Mosaic with only the Fiducial Image Frame module included in
the flow (set run_fiducial_image_frame = 1 if using the command line)
to create a Fiducial Image Frame table that includes all of the images
in the entire input list.
2) Edit the resul...
No, you don't have to redo mosaicking, especially if outlier rejection
is used as part of mosaicking, since APEX does not do outlier
rejection. APEX can use the tiles created by Mosaic and saved in the
coadd directory (COADDER_DIR). If you are using the G...
Yes. If a subdirectory name is specified as a full path, it is not
treated as a subdirectory of OUTPUT_DIR and the name is used as
specified. All you have to do is specify MEDFILTER_DIR to point to the
location where the background-subtracted images creat...
I'm getting the following error message when I run mosaic.pl:
Pipeline Module MOSAIC_COADD Version 2.5
Processing time Tue Jan 20 18:11:26 2004
nmings 10
Error in allocating memory for Coverage Image for Tile 0
mosaic_coadd Error Message 0x0071: MA...
Some Linux users have seen the following error message when trying to
start MOPEX:
Error occurred during initialization of VM
Could not reserve enough space for object heap
Could not create the Java virtual machine.
The MOPEX GUI startup settings a...
The SSC only supports the command-line version of MOPEX on the
following platforms: Solaris 10+, Mac OSX 10.3+ and Linux RedHat. If
you are running a different platform or flavor of Linux then you are
probably experiencing Perl library linking problems (a...
Due to Mac OSX 10.7 (Lion)'s official roll-out being very recent, it
is not among the operating systems currently supported for MOPEX. We
hope to support it in the near future.
Observers attempting to use MOPEX on Lion will get a "PowerPC
applications a...
The command-line and GUI versions of MOPEX (including APEX) are
identical in terms of the results they produce. If you are a new user
then we strongly recommend using the GUI, as it is more user-friendly
and has enhanced, built-in help pages. If you are r...
Parameter Detection_Threshold is probably set too high in the Detect
module. Try lowering it. If this doesn't help, check that your
Min_Coverage parameter isn't higher than the actual coverage in your
mosaic.
The Perl error is most likely a memory limit because you are trying to
derive a PRF from too many stars x too many frames x too big a fitting
area x too fine sampling. For example, if you have a big fitting area,
you could reduce this by lowering PostStam...
Check the uncertainty images - they could be underestimated.
If you are using the GUI then all you need is a set of input images
listed in a text file.
If you are using the command line, you need a set of input images
with their full path name listed in a text file, and you will also
require a "namelist" - a fil...
Any images in the FITS format, but the following keywords are
required:
BITPIX, NAXIS, NAXIS1, NAXIS2, CRVAL1, CRVAL2, CRPIX1, CRPIX2,
CTYPE1, CTYPE2.
Either the CD matrix or CDELT1, CDELT2, CROTA2 keywords are also
required.
There are 3 steps required to use the results of Box Outlier Rejection
in your reduction: 1) add the Mosaic Box Outlier module to your
processing flow (run_mosaic_box_outlier = 1); 2) in the Mosaic RMask
module settings, click the check box for "Use Box O...
For Single Frame Outlier Rejection, the following should be included
(set to 1 in the namelist):
MedFilter (run_medfilter = 1)
Detect RadHit (run_detect_radhit = 1)
For Multiframe Temporal Outlier Rejection the following should be
included (set to 1 ...
Yes. However, many mac owners use the bash shell. In that case, you
must edit one line in each of two files:
line 46 of /smart/utility/misc/sm_list_files.pro
line 81 of /smart/scripts/pro/sc_read_fits_bcd.pro
In each file, the line in question shou...
To do it you need to make your own extraction mask. The simplest way
to do this is to write an IDL routine which makes a 128X128 array,
sets the array elements to the values you want them to be and then
writes out to a file. Mask files can be either ".fit...
Scripted autosky extraction hasn't yet been programmed into SMART and
is on the to do list. However, you could look into the IDL source code
to identify the subroutines which perform source extraction and write
an IDL program which has just these routines...
Read the SMART installation documentation [1] carefully. In almost all
cases, problems have been because of the order of directories in the
IDL_PATH or a missing "+" sign or the absence of the IDL astro library
in the IDL_PATH. Make sure you have the most...
The values that are relevant are RA_SLT, DEC_SLT, PA_SLT. RA_SLT and
DEC_SLT are different for different nod positions while RA_FOV and
DEC_FOV remain the same between nods. So lets say your PA_SLT is 0
degrees (that means the long axis of the slit is rot...
This is a known problem and is being fixed.
It has been reported by a user that selecting 'fixed column'
extraction in the 'interactive extraction' will perform a fixed column
extraction and will use the user-defined extraction width if you
manually set...
Yes, the developers of SMART have written a SMART cookbook [1].
Additional illustrations of data reduction with SMART can be found in
the SMART section of the Spitzer Data Analysis Cookbooks page [2].
Links:
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[1]
http://isc.astro.cornell.edu/smar...
You may encounter the error "Failed during validation" if you have
spaces in the path to your input files. To avoid this problem, you
can:
- remove the space from your path
OR
- identify a directory with no spaces, and create a symbolic link to
your...
Open the "Java Preferences" application, found in Applications >
Utilities > Java, and switch to Java 1.5 32-bit.
If this doesn't work, then close SPICE and open a Terminal window.
Issue the following commands.
cd /Applications/spice/spice.app/Conten...
The aperture shown in CUBISM is data-driven, and does not intend to
represent the full slit. The width in the CUBISM visualization
reflects that of the 1 pixel width wavesamp, which is set that way on
purpose, reflecting the fact that in the cross-slit di...
You may experience inconsistencies between the colors indicated in the
CUBISM documentation and what you see on your screen if you have
chosen to install the full source distribution of CUBISM.
If you have trouble with the colors looking strange on a 1...
In order to understand the answer to this question, you need a little
background on the SSC pipeline. Roughly every six months, the pipeline
number (the "S-number") for all new Spitzer data (from all
instruments) in the archive is incremented as a new sof...
The integrated number counts for sources with flux density of 1 mJy at
24 microns at high latitudes (see Marleau et al. 2004, ApJS, 154, 66)
give 335 sources (both stars and galaxies) per square degree in a high
galactic latitude field. That is one source...
An onboard peak-up algorithm measures the centroid of the brightest
source in the peak-up field. It performs two measurements. First, the
centroid of the brightest source in the peak-up array field-of-view is
measured at an "acquisition" pointing (ACQ). N...
There are two ways for the peak-up to "fail".
1. If the algorithm does not find a valid centroid, then it will
report a failure. In the peak-up images, particularly the processed
DCE (see above), there will be no visible source. You can also
identify th...
An example of the problem using the SH and LH slits is illustrated
here [1].
The spectral map positions are in array coordinates, which have axes
that are parallel and perpendicular to the slit in question. Because
the slits are not exactly parallel (o...
You must add the astrolib library [1] to your IDL path. Make sure that
your IDL path includes SMART before astrolib.
Links:
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[1] http://idlastro.gsfc.nasa.gov/homepage.html
Instructions on how to access your data can be found on the Data
Archives page [1].
Links:
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[1] http://ssc.spitzer.caltech.edu/spitzerdataarchives/
This answer comes in two parts:
* How to reference a Dataset ID in your journal articles [1]
* Guidelines for publication acknowledgments. [2]
Links:
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[1] http://ssc.spitzer.caltech.edu/spitzermission/publications/iau/
[2] http://ssc.spitzer...
To grant someone else access to proprietary data, the primary
investigator (PI) of the program should contact the Spitzer helpdesk
(help@spitzer.caltech.edu [1]) and ask that the person be granted
access. Please include the following information:
* Gr...
No, your _program password_ (aka "Spot password") is not the same as
your _archive password_, sorry!
If you want to access publicly accessible data through the archive,
you do not need a password.
If you want to access proprietary data through th...
We have database blocktime every Thursday from 8 to 10 AM Pacific
time. You may not be able to retrieve data or view programs during
this time because the archive servers are down.
This is a known display issue with Leopard. It applies to IRAC
Post-Cryo AORs only. If you need to know the pipeline version of
post-cryo AORs, please double click on the AOR to open the Detail
Information window, which will display the pipeline version.
This bug happens when using Leopard to find warm mission post cryo
mapping programs. If you de-select IRS and MIPS in the Query: By
Program dialog, no warm mission programs will be returned.
Fix: Select all three instruments in the Query: By Program dia...
Descriptions of all the filenames produced by the different
instruments can be found in the Instrument Handbooks:
* IRAC [1]
* IRS [2]
* MIPS [3]
Links:
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[1] http://ssc.spitzer.caltech.edu/irac/iracinstrumenthandbook/
[2] http://ssc.spitz...
The pbcd products available from the archive were originally intended
as quick-look images of your data. Post-BCD products have been
produced with generic namelists, and the parameters have not been
optimized for your data set. Post-BCD products and Level...
Here are links to pages for each instrument with the filename
conventions and contents spelled out:
* IRAC filenaming scheme [1] - see Section 6.1
* IRS filenaming scheme [2] - see Section 6.1
* MIPS filenaming scheme [3] - see Section 6.2, 6.2.1...
Leopard is now retired as the Spitzer archive interface.
The primary place where you should be downloading Spitzer data is now
the Spitzer Heritage Archive (SHA), which is resident at the NASA/IPAC
Infrared Science Archive (IRSA) at the Infrared Process...
In general, the eight SSC data processing pipelines convert spacecraft
engineering data into scientifically useful data. _Raw data_
(engineering and science) are received at the ground tracking stations
via telemetry and forwarded to the Spitzer Flight Op...
SSC data is electronically accessible as FITS files (no extensions).
The end-product files include complete calibration information and
intermediate files for individual processing 'steps.'
The general philosophy is to do a few things, and do them well! Data
processing for each of the eight pipelines (one per observing mode) is
highly automated. A modular design allows components, or individual
processing steps, to be easily updated. The ...
See the page on DQA Status flag definitions [1].
Links:
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[1] http://ssc.spitzer.caltech.edu/warmmission/scheduling/dqa/
For each AOR, the SSC also provides calibration files, intermediate
data files, quality analysis files, all with complete header
information.
In a nutshell, DATE_OBS is the most accurate, absolute measurement
for comparing with astronomical emphemerides. SCLK_OBS (in real sec)
is good for relative timing comparisons within an AOR or even a
campaign.
More words on this:
* DATE_OBS value...
Pipeline products after S18.5 no longer provide dmasks as they contain
misleading and incomplete information. They have been superceded by
the information contained in the the imask files. The imasks are more
robust, include flagging of various artifacts ...
If you were asking for pointers to documentation, this page [1] is
one-stop-shopping for investigators looking to get started working on
Spitzer data -- archive access, data handbooks, software, data
processing examples, even IAU naming guidelines and ack...
Yes.
Legacy Science Team data is available via the Spitzer Archive
interface or on the web at our Popular Products [1] site.
Data analysis tools are available via our Contributed Software [2]
site.
Links:
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[1] http://data.spitzer.caltech.edu/...
Yes. Because of the large amounts of observing time awarded to
approved Legacy Science teams, and the fact that foreign-based teams
are ineligible for NASA financial support, the proposals from non-US
based proposals were required to submit a credible let...
Yes. In general, the SSC adopts the same approach; that is, to utilize
existing data analysis packages/tools to the maximum extent possible,
and to develop only those unique capabilities required for Spitzer.
No. The proposals were judged based on the technical information
provided on the Spitzer web site, including the Call for Proposals and
the Spitzer Observer's Manual. There was no requirement or need to
include instrument team members or SSC scientists in...
No. The Legacy Science Program has always been identified as a program
that will be based on the best science proposals submitted. THERE WERE
NO PRE-IDENTIFIED SCIENCE AREAS FOR LEGACY SCIENCE. All Legacy science
proposals were judged equally by the Time ...
Yes. There was no restriction on the level of participation of any
scientist. The SSC developed conflict of interest guidelines for its
science staff so that they are aware of the community sensitivities,
and so that the community can be confident that al...
There are three characteristics that distinguish the Spitzer Legacy
Science Program from GO investigations:
* They must be _large coherent_ science investigations, not
reproducible by any reasonable number or combination of smaller
General Observer pro...
The unique and innovative Spitzer Legacy Science Program [1] was
motivated by a desire to enable large observing programs early during
Spitzer's prime mission, with the goal of creating a substantial
database of archived observations that can be utilized ...
Raw and pipeline-processed Legacy Science [1] data from Spitzer enter
the public domain once they are processed and verified at the SSC.
This will typically take up to a few weeks after the observations are
performed. Data are electronically accessible fr...
The Original Legacy Science Program is comprised of six large-scale
peer-reviewed investigations selected in November 2000. The six
approved projects utilize 3160 hours of Spitzer observing time,
primarily in the first year of the mission, and integrate s...
Intermediate and final post-pipeline data products developed by Legacy
Science teams must be delivered to the SSC on a schedule defined by
the team in their proposal. The schedule is consistent with the
boundary conditions described in Section 4.2 and in ...
You need to multiply the values of the pixels by GAIN*EXPTIME/FLUXCONV
to get electrons. These keywords are given in the BCD header. You
should also add a term (-ZODY_EST+SKYDRKZB)/f_ext, where ZODY_EST is
the estimated zodiacal background light at your o...
Most likely the skydark that was subtracted from your data
over-subtracted the background in your images. You can add back the
subtracted skydark background value using the BCD header keyword
SKYDRKZB. See section 6.2 in the IRAC Instrument Handbook. You ...
Yes. Electronic (ASCII) versions of the transmission curves for the
IRAC filters can be found from the IRAC pages [1].
Links:
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[1] http://ssc.spitzer.caltech.edu/irac/
They can be found in Table 4.1 of the IRAC Instrument Handbook. [1].
They are 280.9±4.1 (ch 1), 179.7±2.6 (ch 2), 115.0±1.7 (ch 3) and
64.9±0.9 (ch 4).
Links:
------
[1] http://ssc.spitzer.caltech.edu/irac/iracinstrumenthandbook/
Yes, we are correcting the data for muxbleed and column pulldown in
the pipeline. Sometimes these corrections do not produce a perfect
mitigation of these effects. Therefore, you should always check your
cBCDs and try to perform additional mitigation if n...
We discourage the conversion of IRAC flux densities to IRAC fluxes by
the multiplication with the effective bandwidth since the fluxes
depend on the (unknown) absolute normalization of the instrument
throughput. Instead, you should calculate the flux dens...
There are several things you can do to check for saturation. If you
have HDR data, the saturation flag in the imask file of the long
frames (bit 13) will be set. Similarly the same bit will be set in the
imask if saturation is indicated during linearizati...
You can look up primary calibrators from the Reach et al. (2005) IRAC
calibrator paper and then search for observations of these stars,
constraining your search to the relevant time interval or campaign.
The pixel phase effect will go down as sqrt(number of dithers), so if
it is a 4% effect to start with in channel 1, after combining 5
dithers into a mosaic it should be less than a 2% effect. Of course
you can get even better results by applying the pixel...
Absolute calibration assumes source spectrum F(ν) is proportional to
ν-1. For any other source spectrum, a color correction must be
applied. Corrections are typically a few percent for stellar and
blackbody sources. Corrections can be more significant for...
A so-called labdark is subtracted from each frame, including skydark
frames. So, in simple mathematical terms,
(obj-lab) - (sky-lab) = obj-sky = BCD
where "obj" is a science object frame, "lab" is the appropriate
labdark, and "sky" is an appropriate s...
You want to select the dither pattern in such a way that every part of
your target that is of interest to you will be imaged at least three
times. If your object has spatial variations on a certain large scale,
you will want to select a large enough dithe...
The relationship between Y and Z and IRAC x and y is the following:
+Y = IRAC +x
+Z = IRAC -y
Please see Figure 6.6 in the Spitzer Observer's Manual. It explains
the orientation of the x and y axes and the scattered light boxes with
respect to those ...
The first frame correction in the pipeline has not worked
well for such data. This was sometimes true for channel 3 data
in the cryogenic mission and this is currently always true for warm
IRAC data. The first-order mitigation is fairly simple. Take a ...
Technically challenging observations (e.g., long-term monitoring) may
be converted to Instrument Engineering Requests, IERs, from the
submitted Astronomical Observation Requests, or AORs. To tell whether
your data are from an AOR or IER, look at the BCD h...
The STinyTim PSFs do not work well for IRAC. IRAC pixels are large
relative to the spatial frequencies found in the PSF, and the response
of an IRAC pixel to light varies with position on the pixel. Instead
we recommend the use of the PRFs available on th...
Channel 3 suffers from a large first frame effect. Depending on the
observation strategy, this may cause severe variations in the
background level of the individual BCDs. The effect is worst in frame
repeats (as opposed to frame dithers). To mitigate, you...
Please take a look at the Data Features page [1] and the IRAC
Instrument Handbook [2] which explain what these features are and
shows example images. The pipeline tries to mitigate some of these
artifacts, but the correction is not always perfect. The
art...
You can check the BCD header keyword USEDBPHF. If pointing refinement
ran without problems, it should be set to "T". To see whether the
superboresight pointing refinement ran successfully, you can look at
the value of the BCD header keyword "BPHFNAME." It...
The spectral responses of IRAC are posted on our web pages [1]. You
can use those to figure out the conversions. The STAR-PET [2] also
gives conversions to the K band in different photometric systems for
stars of various types.
Links:
------
[1]
http://s...
Subarray mode is useful for observing very bright sources and/or
observing with high temporal resolution.
In subarray mode, only one corner, 32×32 pixels offset by 8 pixels
from the edges, is read out from one array. Pixels (9:40, 9:40) of the
array ar...
The absolute calibration accuracy for IRAC is discussed in Section 4.3
of the IRAC Instrument Handbook [1] and is 3% for all channels in the
cryogenic mission data, and currently 5% in the warm mission data. The
repeatability is better than 1% for all cha...
The relative accuracy of measuring the separation of two sources in
IRAC images is probably better than 0.3" for source with
signal-to-noise ratio greater than 10 on the same BCD image. One of
the main factors limiting the accuracy is the uncertainty in t...
You could use the SExtractor and the Kron flux from its output. This
was done by the SWIRE Legacy team. Or, you could take a circular
aperture, with a size just larger than the outermost isophote of your
target, and do aperture photometry and apply the ap...
The bias level varies depending on the type of the previous
observation and the time delay between the current and the previous
observation. The variation is highest for very short delays.
Therefore, in-place frame repeats suffer most from this effect. Al...
The pixel phase effect is due to the varying sensitivity of a pixel
across its area. The sensitivity is usually highest in the center of
the pixel. This effect is seen most clearly in channel 1 data, but
appears to exist at a detectable level in channel 2...
In general, users should trust the FLUXCONV values in the headers of
the
IRAC data FITS files that they have. Here is a brief summary of the
changes
in the FLUXCONV values throughout the Spitzer mission.
Warm Mission S18.18 and S19 pipelines:
ch1 FL...
In-place repeats are successive frames taken at the same position, and
dithers move the telescope between pointings. When you move the
telescope, it takes time both for the slew and the subsequent settle
before astronomical observations can begin. (In-pla...
Every IRAC full array AOR with a frame time equal to or greater to 6
seconds will have its first frame taken in the high dynamic range
(HDR) mode. Therefore, you will get one or two short frames before the
long exposure at exactly the same position (see t...
You can get a quick understanding of the various features in your MIPS
data by consulting Chapter 7 in the MIPS Instrument Handbook available
at http://ssc.spitzer.caltech.edu/mips/mipsinstrumenthandbook/ [1]. If
you're analyzing MIPS-Ge (70 and 160 micro...
There is a paragraph in the MIPS Instrument Manual on this very topic.
Now, the 70 micron large field fine pixel scale AOT by default covers
a region about 2.5' x 1.25'. To cover a larger region, you need to use
cluster mode targets to cover the area -- k...
Trying to compare Tables 2.7 and 2.8 is like comparing apples and
oranges. The values for truly (ideal) cases are in Table 2.7. The
formulae in Table 2.8 actually describe the general case, which
includes a combination of point and background flux, so the...
See the discussion at:
http://sha.ipac.caltech.edu/applications/Spitzer/SHA/help/doc/searching.html#byBatch
[1]
Links:
------
[1]
http://sha.ipac.caltech.edu/applications/Spitzer/SHA/help/doc/searching.html#byBatch
The red-shaded data are still proprietary. If they are your data, then
log in and you should be able to download them. If they are not your
data, you can download those data after the data become public,
usually about 12 months after the data were taken (...
Click on the checkbox at the top of the column of checkboxes, at the
top left of the search results pane.
The visualization tools currently only allow you to create 3-color
images that you load from disk or from the web. If you want to create
3-color images using Spitzer data, download the data to disk and then
load them into the SHA from disk as individual c...
Yes, there are a lot more files than what are shown, such as the
errors! We decided for clarity that only certain files of primary
interest to users would appear for individual examination in the SHA
interface, but of course the download includes many mor...
Sometimes, if there is a network hiccup (e.g., you pick up and move
your laptop to a different wireless hub), the SHA can be left in a
funny state. To avoid this, if you've accomplished a complex search,
log in to the SHA and save or tag the search. That ...
When downloading large quantities of data (big programs, whole
campaigns, etc.), the SHA will break up the downloads into
"manageable" pieces, where "manageable" is defined as "not larger than
common computers and software can handle." We understand your
...
72 hours, sometimes longer if the SHA is not under heavy use.
To uncompress the files you have downloaded, type "unzip foo.zip". To
uncompress multiple files at once, type "unzip '*.zip'" (the single
quotes are important), or "unzip \*.zip" -- you just have to escape
out the wildcard.
Each of the instruments (IRAC, IRS, and MIPS) has an Instrument
Handbook, which lists and defines each of the files. They also
describe instrument artifacts, and give guidance as to how to reduce
the data.
If the data was taken in IRAC's subarray mode, or for certain IERs
(Instrument Engineering Requests), there will be no post-BCD data for
the observation. Data in IRAC subarray mode are not processed through
the online post-BCD pipeline. The post-BCD pipel...
The diskette icon will only save the underlying image, not the
overlays. The best way to do this, at this time, is to take a screen
snapshot!
WISE: Wright et al. (2010) [1]
[2]
NEOWISE: Mainzer et al. (2011) [3]
Details on how to acknowledge WISE and NEOWISE are provided in the
documentation [4].
Links:
------
[1] http://adsabs.harvard.edu/abs/2010AJ....140.1868W
[2] http://adsabs.h...
* Data Release 1: Planck Collaboration (2013) [1]
* ERCSC: Planck Collaboration (2011c) [2]
Links:
------
[1] http://planck.caltech.edu/publications2013Results.html
[2]
http://irsa.ipac.caltech.edu/data/Planck/ercsc_v1.3/chary_planck_ercsc.pdf
Spitzer Mission - Werner et al. (2004)
Infrared Array Camera (IRAC) - Fazio et al. (2004)
Infrared Spectrograph (IRS) - Houck et al. (2004)
Multiband Imaging Photometer for Spitzer (MIPS) - Rieke et al. (2004)
Details on how to acknowledge Spitzer...
Skrutskie et al. (2006) [1]
Please include the following standard acknowledgment in any published
material that makes use of 2MASS data products:
_ "This publication makes use of data products from the Two Micron All
Sky Survey, which is a joint pro...
Neugebauer et al. (1984) [1]
Links:
------
[1] http://adsabs.harvard.edu/abs/1984ApJ...278L...1N
Herschel Mission - Pilbratt et al. (2010) [1]
PACS - Poglitsch et al. (2010)
SPIRE - Griffin et al. (2010)
HIFI - de Graauw et al. (2010) [2]
Links:
------
[1] http://adsabs.harvard.edu/abs/2010A%26A...518L...1P
[2] http://adsabs.harvard.edu/abs...
We don't currently have any special Mopex/Apex namelists for crowded
fields. Many people have used the default namelists. If using the GUI,
see Cookbook Recipe 7,
http://irsa.ipac.caltech.edu/data/SPITZER/docs/dataanalysistools/cookbook/7/
[1]. And the...
This usually means that the table you uploaded is in a binary file
format, such as .doc, .rtf or .xls.
In order for a table to be read by IRSA's services, it must be in a
plain text ASCII file. If you are using Microsoft Word, be aware
documents may ap...
This error indicates that the table you uploaded contains too many
data columns and too few column names.
If you are using IPAC ASCII Column-Aligned, or tab- or
comma-delimited formats, the number of cells containing data must not
exceed the number of ...
This error message means that the column names in your table do not
sufficiently describe an object name, or the locations on the sky
using ra, dec, glon, glat, etc.
Clean up the column names so they are recognizable by IRSA services.
See Supported ...
Three common conditions may result in this error message.
REASON #1: When using IPAC Table Format, data are located beneath the
vertical bars in the header.
SOLUTION: Align the data with the columns in the header. (See IPAC
Table Format [1])
R...
REASON: The table is using IPAC ASCII Column-Aligned format, and the
columns are misaligned.
SOLUTION: Make sure the table data are contained within the
boundaries set by the vertical lines in the column header rows.
The GLIMPSE Catalogs null any sources that are bright enough to be in
danger of nonlinear detector response. The GLIMPSE Archives list the
best fluxes that can be measured from such sources despite the
nonlinearity.
Note that the Vizier version of t...
https://www.google.co.in/ [1]
Links:
------
[1] https://www.google.co.in/
This error indicates that you have not entered a search radius. Please
try again with a valid search radius.
In IPAC Table Format, column names can be the combination of
characters, numbers, or underscores ("_"). Blanks, white spaces, tabs,
dashes ("-"), or any other special characters are not allowed as part
of column names. In this case, the parentheses mus...
Your table probably contains a column with data type "int", but with
values that have more digits than allowed by this data type. Try
changing "int" to "long".
For such a long list of Program IDs (PIDs), you will want to write a
script. For each PID, the script should:
1. Search the SHA for all Level 2 products associated with the PID.
For example,
% wget
"http://sha.ipac.caltech.edu/applications/Spitze...
The SMICA maps are multi-extension FITS files containing the CMB (in
the 1st extension) then the residuals at each band in the 2nd and 3rd
extensions. The CMB units are uK_CMB as stated in the headers. For
30-353 GHz the map residuals are map-CMB = for...
For Mac versions starting with Lion and some settings of Gatekeeper,
you may receive the following error message when you try to run SPICE:
"spice" is damaged and can't be opened. You should move it to the
Trash.
Click "Cancel". You will need to te...
IRSA has a mailing list to inform users of new data releases and
tools. Mailings are infrequent; only a few times a year.
If you would like to be added or removed from this email list, please
submit a ticket to the Help Desk.
Here are some tips for making your large catalog search return
faster:
1. If you suspect that your query might return results larger than 2
Gb, you will need to break it up into smaller queries. It can be
difficult to predict the size of the returne...
The IRSA GLIMPSE holdings include Catalogs and Archives. The Catalog
is a MORE RELIABLE list of sources, and the Archive is a MORE COMPLETE
list both in number of sources and flux measurements at each
wavelength (less nulling of fluxes). Vizier has concat...
To retain only the most robust flux densities, apply the following
cuts:
1. Make a SNR cut. Each source has 5 columns ending in "FluxType",
four for each of the IRAC channels and one for MIPS-24. Flux densities
directly detected in an image with SNR...
IRSA is chartered to curate the science products of NASA's infrared
and submillimeter missions, including many large-area and all-sky
surveys. In total, IRSA provides access to more than 20 billion
astronomical measurements, including all-sky coverage ...
To find data for a specific target in IRSA, use our Data Discovery
service [1], which searches science data products across all of IRSA's
data sets based on a target name (e.g., M31) or coordinates (e.g.,
17h44m34s -27d59m13s).
Links:
------
[1] http://i...
You can search IRSA's holdings in several different ways:
1. If you know which source you are interested in, you can see a list
of relevant IRSA data sets by using the Data Discovery Service [1].
2. If you would like to explore the Catalogs gener...
IRSA is part of a larger consortium of projects called the Infrared
Processing and Analysis Center, or IPAC [1], which maintains several
online educational resources for teachers and students, particularly
the Cool Cosmos [2] site.
Additionally, IRS...
If you have data that would benefit the infrared and sub-millimeter
astronomical community, please submit a ticket through IRSA's Help
Desk [1].
To learn more about IRSA's quality standards for contributed data,
please read about IRSA's Data Validat...
Depending on your specific needs, there are a few places you can view
and download presentation-quality images:
The Featured Images Gallery [1] is a gallery of all images featured
on IRSA's home page.
Several 2MASS images are available in the follow...
There are a couple of resources you can tap into:
1. IRSA's Knowledgebase
This is a searchable list of Frequently Asked Questions (FAQs). To
get there, visit the Help Desk at:
https://irsasupport.ipac.caltech.edu/
and click on "Knowledgebas...
IRSA does not routinely provide the ability to download entire data
sets for its mission holdings. In some cases, mission data may have
small enough volume that it is straight-forward to download using
IRSA's program interface. For most missions, however,...
If you are having this problem on a mac, you need to change your
preferences.
Open your System Preferences-->General (under Personal in the top
row).
Set "Show scroll bars" to "Always".
This should fix the problem.
You can find IRAS Zodiacal Observation History files here:
http://sbn.psi.edu/pds/archive/iraszody/ [1]
Or here:
http://lambda.gsfc.nasa.gov/product/iras/zod_o_histfile.cfm [2]
Links:
------
[1] http://sbn.psi.edu/pds/archive/iraszody/
[2] htt...
This is a note about "tune.tbl" files for Spitzer IRS SL1+SL2 (Both)
5.2-14.5 micron spectral mapping, i.e. when the centering was between
the SL1 and SL2 active areas to record the spectra of both ranges
simultaneosly (rather than centering SL1 on a s...
The short answer is that there isn't a WISE Extended Source Catalog.
It is possible to find all WISE sources positionally associated with
2MASS Extended Source Catalog by using IRSA to select AllWISE catalog
sources that have "ext_flg" = 4 or 5. However, ...
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