From 95f95befdfbc14ab5d713ebd8f9b68036cc18f22 Mon Sep 17 00:00:00 2001 From: Jenna Ryon Date: Mon, 1 Jul 2019 18:00:58 -0400 Subject: [PATCH] Update forward model notebook links to new HDox, Jahia, and ADS versions --- .../acs_cte_forward_model_example.ipynb | 20 +++++++++---------- 1 file changed, 10 insertions(+), 10 deletions(-) diff --git a/acs_cte_forward_model/acs_cte_forward_model_example.ipynb b/acs_cte_forward_model/acs_cte_forward_model_example.ipynb index 75c4b3a..1e66ec8 100644 --- a/acs_cte_forward_model/acs_cte_forward_model_example.ipynb +++ b/acs_cte_forward_model/acs_cte_forward_model_example.ipynb @@ -42,9 +42,9 @@ "\n", "The charge transfer efficiency (CTE) of the Advanced Camera for Surveys (ACS) Wide Field Channel (WFC) has been decreasing over the lifetime of the instrument. Radiation damage from cosmic rays and other sources leads to charge traps within the detector. These traps remove electrons from charge packets as they are transferred between rows of the detector, and release the electrons in subsequent pixels. This causes flux to be removed from bright features and released into pixels behind the features (relative to the row closest to the amplifier), creating bright trails.\n", "\n", - "A pixel-based CTE correction model for the ACS/WFC detector is fully described in [Anderson & Bedin (2010)](http://adsabs.harvard.edu/abs/2010PASP..122.1035A), and a recent update to the model is presented in [ACS ISR 2018-04](http://www.stsci.edu/hst/acs/documents/isrs/isr1804.pdf). The model is based on an empirical determination of the number and depth of charge traps distributed across the detector. It simulates detector readout of an input image, removes the result from the input, and iterates five times. In this way, a reverse model is successively approximated by the forward model. Electrons released in trails are removed and added back to the bright feature in which they originated.\n", + "A pixel-based CTE correction model for the ACS/WFC detector is fully described in [Anderson & Bedin (2010)](https://ui.adsabs.harvard.edu/abs/2010PASP..122.1035A/abstract), and a recent update to the model is presented in [ACS ISR 2018-04](http://www.stsci.edu/files/live/sites/www/files/home/hst/instrumentation/acs/documentation/instrument-science-reports-isrs/_documents/isr1804.pdf). The model is based on an empirical determination of the number and depth of charge traps distributed across the detector. It simulates detector readout of an input image, removes the result from the input, and iterates five times. In this way, a reverse model is successively approximated by the forward model. Electrons released in trails are removed and added back to the bright feature in which they originated.\n", "\n", - "The pixel-based correction was implemented in the calibration pipeline code for ACS (`CALACS`) in 2012 and the algorithm was updated and improved in 2018. The CTE correction step within `CALACS` runs on bias-corrected images, `blv_tmp` files, producing `blc_tmp` files, which lack the bright trails due to poor CTE. Further calibration, including dark correction and flat-fielding, produces `flt` and `flc` files from the `blv_tmp` and `blc_tmps` files, respectively. For more information on calibration of ACS/WFC data, see the [ACS Data Handbook](http://www.stsci.edu/hst/acs/documents/handbooks/currentDHB/toc.html).\n", + "The pixel-based correction was implemented in the calibration pipeline code for ACS (`CALACS`) in 2012 and the algorithm was updated and improved in 2018. The CTE correction step within `CALACS` runs on bias-corrected images, `blv_tmp` files, producing `blc_tmp` files, which lack the bright trails due to poor CTE. Further calibration, including dark correction and flat-fielding, produces `flt` and `flc` files from the `blv_tmp` and `blc_tmps` files, respectively. For more information on calibration of ACS/WFC data, see the [ACS Data Handbook](http://www.stsci.edu/files/live/sites/www/files/home/hst/instrumentation/acs/documentation/other-documents/_documents/acs_dhb.pdf).\n", "\n", "Users desiring to more fully understand the effects of pixel-based CTE correction on their science may wish to run the forward model (i.e., the detector readout simulation) on data containing artificial stars. Here we demonstrate two methods for running the CTE forward model. In [Option A](#option-a), we begin with an observed `flc` image, whereas in [Option B](#option_b), we begin with a `raw` image and generate synthetic data on which to run the forward model.\n", "\n", @@ -135,7 +135,7 @@ "\n", "### 2. Download data and reference files\n", "\n", - "Full-frame, new-mode subarray, and 2K old-mode subarray ACS/WFC images can be run through the CTE forward model. New-mode subarrays were added to the HST flight software at the beginning of Cycle 24. These subarrays have `APERTURE` keywords of the type `WFC1A-512, WFC1A-1K, WFC1A-2K`, etc. Old-mode subarrays have `APERTURE` keywords of the type `WFC1-512, WFC1-1K, WFC1-2K`, etc. WFC apertures are also listed in [Table 7.7 of the ACS IHB](http://www.stsci.edu/hst/acs/documents/handbooks/current/c07_obstechniques08.html#368839).\n", + "Full-frame, new-mode subarray, and 2K old-mode subarray ACS/WFC images can be run through the CTE forward model. New-mode subarrays were added to the HST flight software at the beginning of Cycle 24. These subarrays have `APERTURE` keywords of the type `WFC1A-512, WFC1A-1K, WFC1A-2K`, etc. Old-mode subarrays have `APERTURE` keywords of the type `WFC1-512, WFC1-1K, WFC1-2K`, etc. WFC apertures are also listed in [Table 7.7 of the ACS IHB](https://hst-docs.stsci.edu/display/ACSIHB/7.7+ACS+Apertures#id-7.7ACSApertures-table7.7).\n", "\n", "We recommend that the CTE forward model be run on data that has been bias-corrected, but not dark-corrected or flat-fielded. The flat and dark should be present in the image input into the CTE forward model because these features are present in the image when it is read out, and are therefore affected by CTE losses. The forward model can be run on `flc` files, but the results will technically be incorrect. Photometric tests of forward modeled data of both types show minor differences. Post-SM4 subarray data must be destriped with [`acs_destripe_plus`](https://acstools.readthedocs.io/en/latest/acs_destripe_plus.html), which will also perform the other calibration steps. **Note: At this time, `acs_destripe_plus` only produces `flt`/`flc` images.**" ] @@ -290,7 +290,7 @@ "\n", "Users of this notebook may have a preferred method for generating artificial stars and adding them to data, so here we simply add several Gaussians to the image using utilities within `photutils.datasets` in `astropy`. These Gaussians are not representative of the true ACS/WFC PSF, and are added here for illustrative purposes only. Please note that artificial sources with peak values approaching or exceeding the WFC CCD full well value of about 80,000 electrons are not recommended for simulated data. Blooming of charge from saturated pixels is not implemented in this example.\n", "\n", - "There are many tools for generating artificial stars, including [Tiny Tim](http://www.stsci.edu/hst/observatory/focus/TinyTim) (source code may be downloaded [here](http://tinytim.stsci.edu/sourcecode.php)), [effective PSFs](http://www.stsci.edu/hst/acs/documents/isrs/isr0601.pdf), or [`EPSFBuilder`](https://photutils.readthedocs.io/en/stable/epsf.html) in `photutils`. A recent study of PSF models for ACS/WFC can be found [here](http://www.stsci.edu/hst/acs/documents/isrs/isr1708.pdf)." + "There are many tools for generating artificial stars, including [Tiny Tim](http://www.stsci.edu/hst/instrumentation/focus-and-pointing/focus/tiny-tim-hst-psf-modeling), [effective PSFs](http://www.stsci.edu/files/live/sites/www/files/home/hst/instrumentation/acs/documentation/instrument-science-reports-isrs/_documents/isr0601.pdf), or [`EPSFBuilder`](https://photutils.readthedocs.io/en/stable/epsf.html) in `photutils`. A recent study of PSF models for ACS/WFC can be found [here](http://www.stsci.edu/files/live/sites/www/files/home/hst/instrumentation/acs/documentation/instrument-science-reports-isrs/_documents/isr1708.pdf)." ] }, { @@ -894,7 +894,7 @@ "source": [ "Next, obtain the `SCI` extensions of both CCDs. We then multiply by the flat and scale the CTE-corrected dark by a chosen exposure time. We also run the scaled dark image through a Poisson sampler to include Poisson noise in the dark scene. We then add the dark current to the image. If post-flash is desired, multiply the flash reference file by the flash duration, run it through a Poisson sampler, and add to the synthetic data. This is shown in the commented out lines below. We save the result, which is now effectively a `blc_tmp` file. **Note: It is not recommended to use a simulated exposure time that scales pixels in the dark or flash image to or above the full well depth of ~80,000 electrons.**\n", "\n", - "Note that these reference files are specific to the [anneal cycle](http://www.stsci.edu/hst/acs/documents/handbooks/current/c04_detector4.html#415503) in which these data were taken. If an observation date other than that listed in the `DATE-OBS` header keyword is desired for the synthetic data, different reference files will be needed. These can be found by updating the `DATE-OBS` header keyword in the synthetic image to the desired observation date, and rerunning the cell in [Step 2](#download) which uses `CRDS bestrefs` to download the correct reference files." + "Note that these reference files are specific to the anneal cycle in which these data were taken. If an observation date other than that listed in the `DATE-OBS` header keyword is desired for the synthetic data, different reference files will be needed. These can be found by updating the `DATE-OBS` header keyword in the synthetic image to the desired observation date, and rerunning the cell in [Step 2](#download) which uses `CRDS bestrefs` to download the correct reference files." ] }, { @@ -1248,9 +1248,9 @@ "source": [ "### For more help:\n", "\n", - "More details may be found on the [ACS website](http://www.stsci.edu/hst/acs) and in the [ACS Instrument](http://www.stsci.edu/hst/acs/documents/handbooks/current/cover.html) and [Data Handbooks](http://www.stsci.edu/hst/acs/documents/handbooks/currentDHB/acs_cover.html).\n", + "More details may be found on the [ACS website](http://www.stsci.edu/hst/instrumentation/acs) and in the [ACS Instrument](https://hst-docs.stsci.edu/display/ACSIHB) and [Data Handbooks](http://www.stsci.edu/files/live/sites/www/files/home/hst/instrumentation/acs/documentation/other-documents/_documents/acs_dhb.pdf).\n", "\n", - "Please visit the [HST Help Desk](hsthelp.stsci.edu). Through the help desk portal, you can explore the HST Knowledge Base and request additional help from experts." + "Please visit the [HST Help Desk](http://hsthelp.stsci.edu). Through the help desk portal, you can explore the HST Knowledge Base and request additional help from experts." ] }, { @@ -1274,9 +1274,9 @@ "metadata": { "anaconda-cloud": {}, "kernelspec": { - "display_name": "Python [conda env:astroconda]", + "display_name": "Python 3", "language": "python", - "name": "conda-env-astroconda-py" + "name": "python3" }, "language_info": { "codemirror_mode": { @@ -1288,7 +1288,7 @@ "name": "python", "nbconvert_exporter": "python", "pygments_lexer": "ipython3", - "version": "3.5.5" + "version": "3.6.7" } }, "nbformat": 4,