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Start Over Subject small magellanic cloud Validation Level 2 Capability Type Table Access Protocol
1. SAGE-SMC IRAC Epoch 1 Archive
ID:
ivo://irsa.ipac/Spitzer/Catalog/SAGE-SMC/SAGESMC-IEp1Ar
Title:
SAGE-SMC IRAC Epoch 1 Archive
Short Name:
SAGESMC-IEp1Ar
Date:
01 Oct 2018 20:27:18
Publisher:
NASA/IPAC Infrared Science Archive
Description:
The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. In comparison to the catalog, the archive has more source fluxes (fewer nulled wavelengths) and some more sources but these additions have more uncertainty associated with them. For the catalog, a source must be detected in at least 60% of the observations at that wavelength, at least 32% of the observations in an adjacent band (the confirming band), and the S/N must be greater than [5, 5, 5, 7] for IRAC bands [3.6um], [4.5um], [5.8um] and [8.0um]. The 2MASS K_s band is counted as a detection. For a typical source, extracted from 2x12 sec frametime images, the minimum detection criterion amounts to being detected twice in one band (usually band 1 or 2) and once in an adjacent band (sometimes referred to as the 2+1 criterion). For the catalog, sources with neighbors within a 2" radius are excluded (culled). For the archive, sources within a 0.5" are excluded. For more details, see Section 3.3 of the SAGE-SMC Data Delivery Document.
2. SAGE-SMC IRAC Epoch 1 Catalog
ID:
ivo://irsa.ipac/Spitzer/Catalog/SAGE-SMC/SAGESMC-IEp1Cat
Title:
SAGE-SMC IRAC Epoch 1 Catalog
Short Name:
SAGESMC-IEp1Cat
Date:
01 Oct 2018 20:27:18
Publisher:
NASA/IPAC Infrared Science Archive
Description:
The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. In comparison to the catalog, the archive has more source fluxes (fewer nulled wavelengths) and some more sources but these additions have more uncertainty associated with them. For the catalog, a source must be detected in at least 60% of the observations at that wavelength, at least 32% of the observations in an adjacent band (the confirming band), and the S/N must be greater than [5, 5, 5, 7] for IRAC bands [3.6um], [4.5um], [5.8um] and [8.0um]. The 2MASS K_s band is counted as a detection. For a typical source, extracted from 2x12 sec frametime images, the minimum detection criterion amounts to being detected twice in one band (usually band 1 or 2) and once in an adjacent band (sometimes referred to as the 2+1 criterion). For the catalog, sources with neighbors within a 2" radius are excluded (culled). For the archive, sources within a 0.5" are excluded. For more details, see Section 3.3 of the SAGE-SMC Data Delivery Document.
3. SAGE-SMC IRAC Epoch 0, Epoch 1, and Epoch 2 Archive
ID:
ivo://irsa.ipac/Spitzer/Catalog/SAGE-SMC/SAGESMC-IMEAr
Title:
SAGE-SMC IRAC Epoch 0, Epoch 1, and Epoch 2 Archive
Short Name:
SAGESMC-IMEAr
Date:
01 Oct 2018 20:27:18
Publisher:
NASA/IPAC Infrared Science Archive
Description:
The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. In comparison to the catalog, the archive has more source fluxes (fewer nulled wavelengths) and some more sources but these additions have more uncertainty associated with them. For the catalog, a source must be detected in at least 60% of the observations at that wavelength, at least 32% of the observations in an adjacent band (the confirming band), and the S/N must be greater than [5, 5, 5, 7] for IRAC bands [3.6um], [4.5um], [5.8um] and [8.0um]. The 2MASS K_s band is counted as a detection. For a typical source, extracted from 2x12 sec frametime images, the minimum detection criterion amounts to being detected twice in one band (usually band 1 or 2) and once in an adjacent band (sometimes referred to as the 2+1 criterion). For the catalog, sources with neighbors within a 2" radius are excluded (culled). For the archive, sources within a 0.5" are excluded. For more details, see Section 3.3 of the SAGE-SMC Data Delivery Document.
4. SAGE-SMC IRAC Epoch 0, Epoch 1, and Epoch 2 Catalog
ID:
ivo://irsa.ipac/Spitzer/Catalog/SAGE-SMC/SAGESMC-IMECat
Title:
SAGE-SMC IRAC Epoch 0, Epoch 1, and Epoch 2 Catalog
Short Name:
SAGESMC-IMECat
Date:
01 Oct 2018 20:27:18
Publisher:
NASA/IPAC Infrared Science Archive
Description:
The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. In comparison to the catalog, the archive has more source fluxes (fewer nulled wavelengths) and some more sources but these additions have more uncertainty associated with them. For the catalog, a source must be detected in at least 60% of the observations at that wavelength, at least 32% of the observations in an adjacent band (the confirming band), and the S/N must be greater than [5, 5, 5, 7] for IRAC bands [3.6um], [4.5um], [5.8um] and [8.0um]. The 2MASS K_s band is counted as a detection. For a typical source, extracted from 2x12 sec frametime images, the minimum detection criterion amounts to being detected twice in one band (usually band 1 or 2) and once in an adjacent band (sometimes referred to as the 2+1 criterion). For the catalog, sources with neighbors within a 2" radius are excluded (culled). For the archive, sources within a 0.5" are excluded. For more details, see Section 3.3 of the SAGE-SMC Data Delivery Document.
5. SAGE-SMC IRAC Single Frame + Mosaic Photometry Archive
ID:
ivo://irsa.ipac/Spitzer/Catalog/SAGE-SMC/SAGESMC-IRACAr
Title:
SAGE-SMC IRAC Single Frame + Mosaic Photometry Archive
Short Name:
SAGESMC-IRACAr
Date:
01 Oct 2018 20:27:18
Publisher:
NASA/IPAC Infrared Science Archive
Description:
The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. In comparison to the catalog, the archive has more source fluxes (fewer nulled wavelengths) and some more sources but these additions have more uncertainty associated with them. For the catalog, a source must be detected in at least 60% of the observations at that wavelength, at least 32% of the observations in an adjacent band (the confirming band), and the S/N must be greater than [5, 5, 5, 7] for IRAC bands [3.6um], [4.5um], [5.8um] and [8.0um]. The 2MASS K_s band is counted as a detection. For a typical source, extracted from 2x12 sec frametime images, the minimum detection criterion amounts to being detected twice in one band (usually band 1 or 2) and once in an adjacent band (sometimes referred to as the 2+1 criterion). For the catalog, sources with neighbors within a 2" radius are excluded (culled). For the archive, sources within a 0.5" are excluded. For more details, see Section 3.3 of the SAGE-SMC Data Delivery Document.
6. SAGE-SMC IRAC Single Frame + Mosaic Photometry Catalog
ID:
ivo://irsa.ipac/Spitzer/Catalog/SAGE-SMC/SAGESMC-IRACCat
Title:
SAGE-SMC IRAC Single Frame + Mosaic Photometry Catalog
Short Name:
SAGESMC-IRACCat
Date:
01 Oct 2018 20:27:18
Publisher:
NASA/IPAC Infrared Science Archive
Description:
The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. In comparison to the catalog, the archive has more source fluxes (fewer nulled wavelengths) and some more sources but these additions have more uncertainty associated with them. For the catalog, a source must be detected in at least 60% of the observations at that wavelength, at least 32% of the observations in an adjacent band (the confirming band), and the S/N must be greater than [5, 5, 5, 7] for IRAC bands [3.6um], [4.5um], [5.8um] and [8.0um]. The 2MASS K_s band is counted as a detection. For a typical source, extracted from 2x12 sec frametime images, the minimum detection criterion amounts to being detected twice in one band (usually band 1 or 2) and once in an adjacent band (sometimes referred to as the 2+1 criterion). For the catalog, sources with neighbors within a 2" radius are excluded (culled). For the archive, sources within a 0.5" are excluded. For more details, see Section 3.3 of the SAGE-SMC Data Delivery Document.
7. SAGE-SMC MIPS 70 micron Combined Epoch Catalog
ID:
ivo://irsa.ipac/Spitzer/Catalog/SAGE-SMC/SAGESMC-M2Cat
Title:
SAGE-SMC MIPS 70 micron Combined Epoch Catalog
Short Name:
SAGESMC-M2Cat
Date:
01 Oct 2018 20:27:18
Publisher:
NASA/IPAC Infrared Science Archive
Description:
The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. To be included in each single epoch catalog, each 24 um source has to meet a number of criteria. The source had to be nearly point like with a correlation value >0.89. This removed approximately 2/3 of the entries in the single epoch source lists. In regions where there is a significant structure in the surrounding region (identified as having a sigma > 0.25 in a 120" width square box), the source had to have a correlation value >0.91. This requirement removed a small number of sources (70). Finally, all sources had to have signal-to-noise (S/N) values >5. The S/N used was that estimated from the StarFinder code using the mosaic uncertainty image added in quadrature with an 0.6% error due to the background subtraction. This removed 700 sources. The final Epoch 1 catalog likely has a few remaining unreliable sources, estimated to be at less than the 1% level. The Full List contains ALL sources extracted from the MIPS 24 um mosaics, thus a user should be aware that it contains spurious sources. For more details, see Section 4.1 of the SAGE-SMC Data Delivery Document.
8. SAGE-SMC MIPS 160 micron Combined Epoch Catalog
ID:
ivo://irsa.ipac/Spitzer/Catalog/SAGE-SMC/SAGESMC-M3Cat
Title:
SAGE-SMC MIPS 160 micron Combined Epoch Catalog
Short Name:
SAGESMC-M3Cat
Date:
01 Oct 2018 20:27:18
Publisher:
NASA/IPAC Infrared Science Archive
Description:
The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. To be included in each single epoch catalog, each 24 um source has to meet a number of criteria. The source had to be nearly point like with a correlation value >0.89. This removed approximately 2/3 of the entries in the single epoch source lists. In regions where there is a significant structure in the surrounding region (identified as having a sigma > 0.25 in a 120" width square box), the source had to have a correlation value >0.91. This requirement removed a small number of sources (70). Finally, all sources had to have signal-to-noise (S/N) values >5. The S/N used was that estimated from the StarFinder code using the mosaic uncertainty image added in quadrature with an 0.6% error due to the background subtraction. This removed 700 sources. The final Epoch 1 catalog likely has a few remaining unreliable sources, estimated to be at less than the 1% level. The Full List contains ALL sources extracted from the MIPS 24 um mosaics, thus a user should be aware that it contains spurious sources. For more details, see Section 4.1 of the SAGE-SMC Data Delivery Document.
9. SAGE-SMC MIPS 160 micron Combined Epoch Full List
ID:
ivo://irsa.ipac/Spitzer/Catalog/SAGE-SMC/SAGESMC-M3Full
Title:
SAGE-SMC MIPS 160 micron Combined Epoch Full List
Short Name:
SAGESMC-M3Full
Date:
01 Oct 2018 20:27:18
Publisher:
NASA/IPAC Infrared Science Archive
Description:
The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. To be included in each single epoch catalog, each 24 um source has to meet a number of criteria. The source had to be nearly point like with a correlation value >0.89. This removed approximately 2/3 of the entries in the single epoch source lists. In regions where there is a significant structure in the surrounding region (identified as having a sigma > 0.25 in a 120" width square box), the source had to have a correlation value >0.91. This requirement removed a small number of sources (70). Finally, all sources had to have signal-to-noise (S/N) values >5. The S/N used was that estimated from the StarFinder code using the mosaic uncertainty image added in quadrature with an 0.6% error due to the background subtraction. This removed 700 sources. The final Epoch 1 catalog likely has a few remaining unreliable sources, estimated to be at less than the 1% level. The Full List contains ALL sources extracted from the MIPS 24 um mosaics, thus a user should be aware that it contains spurious sources. For more details, see Section 4.1 of the SAGE-SMC Data Delivery Document.
10. SAGE-SMC MIPS 70 micron Combined Epoch Full List
ID:
ivo://irsa.ipac/Spitzer/Catalog/SAGE-SMC/SAGESMC-M2Full
Title:
SAGE-SMC MIPS 70 micron Combined Epoch Full List
Short Name:
SAGESMC-M2Full
Date:
01 Oct 2018 20:27:18
Publisher:
NASA/IPAC Infrared Science Archive
Description:
The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. To be included in each single epoch catalog, each 24 um source has to meet a number of criteria. The source had to be nearly point like with a correlation value >0.89. This removed approximately 2/3 of the entries in the single epoch source lists. In regions where there is a significant structure in the surrounding region (identified as having a sigma > 0.25 in a 120" width square box), the source had to have a correlation value >0.91. This requirement removed a small number of sources (70). Finally, all sources had to have signal-to-noise (S/N) values >5. The S/N used was that estimated from the StarFinder code using the mosaic uncertainty image added in quadrature with an 0.6% error due to the background subtraction. This removed 700 sources. The final Epoch 1 catalog likely has a few remaining unreliable sources, estimated to be at less than the 1% level. The Full List contains ALL sources extracted from the MIPS 24 um mosaics, thus a user should be aware that it contains spurious sources. For more details, see Section 4.1 of the SAGE-SMC Data Delivery Document.

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