MACHO Project: Variable Star Catalog Lightcurve Selection Help
Index
| Lightcurve Selection | |
|---|---|
| 1.0 Query | |
| 2.0 Hit Count | |
| 3.0 Navigation | |
| 3.1 Using `Back' | |
| 3.2 Help | |
| 3.3 New Search | |
| 3.4 Templates | |
| 3.5 Previous | |
| 3.6 Next | |
| 3.7 ftp Bundle | |
| 4.0 Summary Table | |
| 4.1 View Lightcurve | |
| 4.2 Field.Tile.Seqn | |
| 4.3 Location (J2000) | |
| 4.4 Variability Index | |
| 4.5 Classification | |
| 4.6 # Obs | |
| 4.7 Obs w/2 Pts | |
| 4.8 Focal Plane | |
| 4.9 Pts | |
| 4.10 Period (Days) | |
| 4.12 Magnitude Ave (K-C) | |
| 4.13 Amplitude Ave | |
| 4.14 Sup RSA | |
| 4.15 Sig | |
| 4.16 Chi2r | |
Lightcurve Selection
1.0 Query
The first block in the Lightcurve (LC) Selection page displays the query,
which was reformatted into Concise CommandLanguage syntax.
Refer here for
more information on the CCL syntax and the LC database fields' names. Note that
the database manager does not support floating point search keys, so affected
fields have been multiplied by an appropriate factor to convert to the data
to integer.
2.0 Hit Count
The total number of database records matching the search query is displayed
in the second block. The number of records displayed per page is
limited to the number requested on the query form. To scan through all
matching records, click on either
Previous or
Next.
3.0 Navigation
3.1 Using `Back'
The Back browser button generally should not be used to return to the
Variable Star Catalog query form since the previous page is actually the transient
jump-through prior to the summary page's display. Using Back
will cause the redisplay of the same summary page. If you're really fast on
the click, you can sometimes jump back twice in order to reach the query page.
It's much easier to select New Search though.
3.2 Help
Help displays this document.
3.3 New Search
New Search redirects the browser to a new Lightcurve query form.
3.4 Templates
Templates redirects the browser to the Macho Domain,
Field, and Template Image specifications. The Template Image identifier is
provided as an ftp link to the relevant observation image.
3.5 Previous
Previous redirects the browser to the block of summary records
preceding the current display.
3.6 Next
Next redirects the browser to the block of summary records immediately
following the current display.
3.7 ftp Bundle
ftp Bundle initiates the immediate ftp of the selected
lightcurves bundled in a Unix tar file.
4.0 Summary Table
The table contains attribute data on lightcurves matching the search query.
The attribute data includes a lightcurve's Macho Project Identifier,
observation details, and various statistics generated when determining its
variablity classification.
The table's clickable fields initiate either:
a lightcurve browser and extracter or
selection for later batch retrieval of multiple lightcurve's data (Bundle).
4.1 View Lightcurve
A lightcurve browser is invoked to display the selected lightcurve. The
tool provides a myriad of options such as zoom in/out, list a single
observation's data, list the entire lightcurve's data, display phase data
in addition to photomety data, alter units of display.
A secondary browser window is opened for lightcurve display; it is
used for all lightcurve browsing.
4.2 Field.Tile.Seqn
The Macho Project identifier for the star consisting of the
Macho Field, Tile, and Sequence identifiers for an individual star.
Refer here for the
Macho Field definitions.
4.3 Location
RA : Right Ascension of star in J2000 coordinates.
Dec : Declination of star in J2000 coordinates.
4.4 Variability Index
Variability index from Pierce et al, 1994, Nature 371:385
4.5 Classification
Classification of variable star based on statistical analysis
of its photometry over time.
The classifications follow:
0 : unknown : undefined classification
1 : RRL AB : RRLyrae ab
2 : RRL C : RRLyrae c
3 : RRL E : RRLyrae e
4 : Ceph Fund : Cepheid fundamental
5 : Ceph 1st : Cepheid first overtone
6 : LPV WoodA : LPV Wood-A
7 : LPV WoodB : LPV Wood-B
8 : LPV WoodC : LPV Wood-C
9 : LPV WoodD : LPV Wood-D
10 : EB : Eclipsing Binary (all kinds including Wood-E)
-- default
11 : RRL + GB : RR Lyrae and GB blends (supersedes
Cepheid first overtone in overlap region)
4.6 # Obs
Number of observations collecting data from either both or one
focal plane.
4.7 Obs w/2 Pts
Number of observations where the star was observed simultaneously
in both focal planes.
4.8 Focal Plane
Indicates the relevant focal plane, red or blue, for the subsequent
attributes in the summary table. Refer to Alves paper on calibration
for a thourough discussion of the Macho focal plane characteristics.
4.9 # Pts
Number of observations taken using the relevant focal plane.
4.10 Period (Days)
Average Period is selected as the best 1 cycle period that matches
the alternate focal plane's period. Units are days.
A value of -999 indicates data was taken on only one focal plane.
4.12 Magnitude Ave (K-C)
Magnitude averaged over all observations excepting those with
values of -99, or magnitudes brighter than -12, or type outside of 1-6 or 21-26.
A simple pair of photometric transformations which ignores differences in
aperture corrections from template field to template field was used to
approximate Kron-Cousins V and R photometry. The equations used were:
$mag_ave_bminusr = $bmagave - $rmagave;
$mag_ave_V = $bmagave + 24.32 - 0.18 * ($bmagave - $rmagave);
$mag_ave_R = $rmagave + 24.06 - 0.18 * ($bmagave - $rmagave);
$mag_ave_KVminusKR = $mag_ave_V - $mag_ave_R;
For more accurate transformations for a given star, consult Alcock, C.
et al. 1999, PASP, 111, 1539.
4.13 Amplitude Ave
Average Amplitude is the peak-to-peak amplitude of the best fit
to the light curve.
4.14 Sup RSA
Sup RSA is the weighted mean absolute deviation of the data
from the fit to the light curve. The weighting is such that good
fits typically have values less than 1.0
A value of -999 indicates invalid data.
4.15 Sig
Sig is the standard deviation of the focal plane's magnitude.
A value of -99 indicates invalid data.
4.16 Chi2r
Chi2r is a robust, weighted mean-square difference of the data
and the fit. Only the central 80% of the differences are used in
forming chi2r.
Acknowledgement to use when referencing MACHO Project data
"This paper utilizes public domain data originally obtained by the MACHO Project,
whose work was performed under the joint auspices of
the U.S. Department of Energy, National Nuclear Security Administration by the
University of California, Lawrence Livermore National Laboratory under contract No.
W-7405-Eng-48,
the National Science Foundation through the Center for Particle Astrophysics of the
University of California under cooperative agreement AST-8809616, and
the Mount Stromlo and Siding Spring Observatory, part of the Australian National University."
email enquiries
and 
3.0 Navigation
3.1 Using `Back'
The Back browser button generally should not be used to return to the
Variable Star Catalog query form since the previous page is actually the transient
jump-through prior to the summary page's display. Using Back
will cause the redisplay of the same summary page. If you're really fast on
the click, you can sometimes jump back twice in order to reach the query page.
It's much easier to select New Search though.
3.2 Help
Help displays this document.
3.3 New Search
New Search redirects the browser to a new Lightcurve query form.
3.4 Templates
Templates redirects the browser to the Macho Domain,
Field, and Template Image specifications. The Template Image identifier is
provided as an ftp link to the relevant observation image.
3.5 Previous
Previous redirects the browser to the block of summary records
preceding the current display.
3.6 Next
Next redirects the browser to the block of summary records immediately
following the current display.
3.7 ftp Bundle
ftp Bundle initiates the immediate ftp of the selected
lightcurves bundled in a Unix tar file.
4.0 Summary Table
The table contains attribute data on lightcurves matching the search query.
The attribute data includes a lightcurve's Macho Project Identifier,
observation details, and various statistics generated when determining its
variablity classification.
The table's clickable fields initiate either:
a lightcurve browser and extracter or
selection for later batch retrieval of multiple lightcurve's data (Bundle).
4.1 View Lightcurve
A lightcurve browser is invoked to display the selected lightcurve. The
tool provides a myriad of options such as zoom in/out, list a single
observation's data, list the entire lightcurve's data, display phase data
in addition to photomety data, alter units of display.
A secondary browser window is opened for lightcurve display; it is
used for all lightcurve browsing.
4.2 Field.Tile.Seqn
The Macho Project identifier for the star consisting of the
Macho Field, Tile, and Sequence identifiers for an individual star.
Refer here for the
Macho Field definitions.
4.3 Location
RA : Right Ascension of star in J2000 coordinates.
Dec : Declination of star in J2000 coordinates.
4.4 Variability Index
Variability index from Pierce et al, 1994, Nature 371:385
4.5 Classification
Classification of variable star based on statistical analysis
of its photometry over time.
The classifications follow:
0 : unknown : undefined classification
1 : RRL AB : RRLyrae ab
2 : RRL C : RRLyrae c
3 : RRL E : RRLyrae e
4 : Ceph Fund : Cepheid fundamental
5 : Ceph 1st : Cepheid first overtone
6 : LPV WoodA : LPV Wood-A
7 : LPV WoodB : LPV Wood-B
8 : LPV WoodC : LPV Wood-C
9 : LPV WoodD : LPV Wood-D
10 : EB : Eclipsing Binary (all kinds including Wood-E)
-- default
11 : RRL + GB : RR Lyrae and GB blends (supersedes
Cepheid first overtone in overlap region)
4.6 # Obs
Number of observations collecting data from either both or one
focal plane.
4.7 Obs w/2 Pts
Number of observations where the star was observed simultaneously
in both focal planes.
4.8 Focal Plane
Indicates the relevant focal plane, red or blue, for the subsequent
attributes in the summary table. Refer to Alves paper on calibration
for a thourough discussion of the Macho focal plane characteristics.
4.9 # Pts
Number of observations taken using the relevant focal plane.
4.10 Period (Days)
Average Period is selected as the best 1 cycle period that matches
the alternate focal plane's period. Units are days.
A value of -999 indicates data was taken on only one focal plane.
4.12 Magnitude Ave (K-C)
Magnitude averaged over all observations excepting those with
values of -99, or magnitudes brighter than -12, or type outside of 1-6 or 21-26.
A simple pair of photometric transformations which ignores differences in
aperture corrections from template field to template field was used to
approximate Kron-Cousins V and R photometry. The equations used were:
$mag_ave_bminusr = $bmagave - $rmagave;
$mag_ave_V = $bmagave + 24.32 - 0.18 * ($bmagave - $rmagave);
$mag_ave_R = $rmagave + 24.06 - 0.18 * ($bmagave - $rmagave);
$mag_ave_KVminusKR = $mag_ave_V - $mag_ave_R;
For more accurate transformations for a given star, consult Alcock, C.
et al. 1999, PASP, 111, 1539.
4.13 Amplitude Ave
Average Amplitude is the peak-to-peak amplitude of the best fit
to the light curve.
4.14 Sup RSA
Sup RSA is the weighted mean absolute deviation of the data
from the fit to the light curve. The weighting is such that good
fits typically have values less than 1.0
A value of -999 indicates invalid data.
4.15 Sig
Sig is the standard deviation of the focal plane's magnitude.
A value of -99 indicates invalid data.
4.16 Chi2r
Chi2r is a robust, weighted mean-square difference of the data
and the fit. Only the central 80% of the differences are used in
forming chi2r.
Acknowledgement to use when referencing MACHO Project data
"This paper utilizes public domain data originally obtained by the MACHO Project,
whose work was performed under the joint auspices of
the U.S. Department of Energy, National Nuclear Security Administration by the
University of California, Lawrence Livermore National Laboratory under contract No.
W-7405-Eng-48,
the National Science Foundation through the Center for Particle Astrophysics of the
University of California under cooperative agreement AST-8809616, and
the Mount Stromlo and Siding Spring Observatory, part of the Australian National University."
email enquiries
and
The table's clickable fields initiate either:
4.1 View Lightcurve
A lightcurve browser is invoked to display the selected lightcurve. The tool provides a myriad of options such as zoom in/out, list a single observation's data, list the entire lightcurve's data, display phase data in addition to photomety data, alter units of display.
A secondary browser window is opened for lightcurve display; it is used for all lightcurve browsing.
4.2 Field.Tile.Seqn
The Macho Project identifier for the star consisting of the Macho Field, Tile, and Sequence identifiers for an individual star. Refer here for the Macho Field definitions.
4.3 Location
4.4 Variability Index
Variability index from Pierce et al, 1994, Nature 371:385
4.5 Classification
Classification of variable star based on statistical analysis
of its photometry over time.
The classifications follow:
0 : unknown : undefined classification
1 : RRL AB : RRLyrae ab
2 : RRL C : RRLyrae c
3 : RRL E : RRLyrae e
4 : Ceph Fund : Cepheid fundamental
5 : Ceph 1st : Cepheid first overtone
6 : LPV WoodA : LPV Wood-A
7 : LPV WoodB : LPV Wood-B
8 : LPV WoodC : LPV Wood-C
9 : LPV WoodD : LPV Wood-D
10 : EB : Eclipsing Binary (all kinds including Wood-E)
-- default
11 : RRL + GB : RR Lyrae and GB blends (supersedes
Cepheid first overtone in overlap region)
4.6 # Obs
Number of observations collecting data from either both or one focal plane.
4.7 Obs w/2 Pts
Number of observations where the star was observed simultaneously in both focal planes.
4.8 Focal Plane
Indicates the relevant focal plane, red or blue, for the subsequent attributes in the summary table. Refer to Alves paper on calibration for a thourough discussion of the Macho focal plane characteristics.
4.9 # Pts
Number of observations taken using the relevant focal plane.
4.10 Period (Days)
Average Period is selected as the best 1 cycle period that matches the alternate focal plane's period. Units are days.
A value of -999 indicates data was taken on only one focal plane.
4.12 Magnitude Ave (K-C)
Magnitude averaged over all observations excepting those with values of -99, or magnitudes brighter than -12, or type outside of 1-6 or 21-26.
A simple pair of photometric transformations which ignores differences in
aperture corrections from template field to template field was used to
approximate Kron-Cousins V and R photometry. The equations used were:
$mag_ave_bminusr = $bmagave - $rmagave;
$mag_ave_V = $bmagave + 24.32 - 0.18 * ($bmagave - $rmagave);
$mag_ave_R = $rmagave + 24.06 - 0.18 * ($bmagave - $rmagave);
$mag_ave_KVminusKR = $mag_ave_V - $mag_ave_R;
For more accurate transformations for a given star, consult Alcock, C. et al. 1999, PASP, 111, 1539.
4.13 Amplitude Ave
Average Amplitude is the peak-to-peak amplitude of the best fit to the light curve.
4.14 Sup RSA
Sup RSA is the weighted mean absolute deviation of the data
from the fit to the light curve. The weighting is such that good
fits typically have values less than 1.0
A value of -999 indicates invalid data.
4.15 Sig
Sig is the standard deviation of the focal plane's magnitude. A value of -99 indicates invalid data.
4.16 Chi2r
Chi2r is a robust, weighted mean-square difference of the data and the fit. Only the central 80% of the differences are used in forming chi2r.
Acknowledgement to use when referencing MACHO Project data
"This paper utilizes public domain data originally obtained by the MACHO Project,
whose work was performed under the joint auspices of
the U.S. Department of Energy, National Nuclear Security Administration by the
University of California, Lawrence Livermore National Laboratory under contract No.
W-7405-Eng-48,
the National Science Foundation through the Center for Particle Astrophysics of the
University of California under cooperative agreement AST-8809616, and
the Mount Stromlo and Siding Spring Observatory, part of the Australian National University."
and