0Assigned ID: 534
----- Attempting Submission 1 (Fri Mar 06 16:27:58 GMT 2020) -----
HST Phase I Proposal 534 successfully submitted.
Receipt: # 534-1COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant.
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browserThis is a resubmission to retake failure in Visit 14.-2100554624----- Attempting Submission 1 (Mon Jun 29 15:31:54 GMT 2020) -----
HST Phase II Proposal 16260 successfully submitted.
Receipt: # 16260-1
----- Attempting Submission 2 (Wed Feb 17 18:32:00 GMT 2021) -----
----- Attempting Submission 3 (Thu May 27 15:02:58 GMT 2021) -----
HST Phase II Proposal 16260 successfully submitted.
Receipt: # 16260-3
----- Attempting Submission 4 (Fri Dec 10 18:39:00 GMT 2021) -----COS extended target warning: We will be performing custom calibration and extraction on all of of our COS observations.
This will be done by Co-I Svea Hernandez who is an expert with COS data and dark current calibrations.
FLASH level: We are following the value recommended by email from STScI.
POS TARG with Quad Filter: The offsets are only a very small manual dither to optimize spatial resolution.Tied up in Knots: The Spatially Resolved LyC Escape from Haro 11The nearest and most well-studied Lyman continuum (LyC) emitting galaxy, Haro 11, offers an unparalleled opportunity to determine the conditions for LyC escape at 15-pc resolution. However, we do not know which of the 3 dominant star-forming knots is the LyC source: Knot C is a strong Ly-alpha emitter (LAE) with an ultraluminous X-ray source (ULX); Knot B hosts a very luminous ULX that is a candidate low-luminosity AGN (LLAGN); and Knot A is a starburst driving optically thin, Green Pea-like properties. Our proposed COS spectra of the LyC will identify which of the three knots is responsible for the known LyC emission. Depending on which Knot is confirmed as the LyC emitter (LCE), it would illuminate the connection between LyC escape and: LAEs and ULXs (Knot C); ULXs/LLAGN (Knot B); or Green Peas (Knot A). If Knot C is not confirmed, then this would overturn the widely held paradigm that all LCEs must be strong LAEs. If Knot B or C is the LyC source, then this first confirmation of a ULX LCE would imply that black hole accretion processes in dwarf galaxies may be a viable cosmological source of LyC. By establishing the LyC source in this iconic galaxy, these observations will allow much-needed, spatially resolved, detailed study of the radiative transfer of LyC from the ionizing source through the local ISM. Our results will clarify understanding of LyC escape and its relation to Ly-alpha, and inform efforts to identify LCEs at higher redshift.We will obtain COS LyC spectral observations using G130M/1055, of the three separate targets, Knots A, B, and C, within Haro 11, to determine which of the three is the LyC emitter. With redshift z = 0.021, the 912 A Lyman break of Haro 11 falls at 931 A. We will observe uncontaminated Haro 11 LyC emission in a 3.4 A window between the 930.75 A and 926.25 A geocoronal lines, and in a 2.0 A window between the 926.25 A and 923.15 A geocoronal lines. The exposure times for all 3 Knots are identical, ~14 ks, or 6 orbits each.
COS has previously observed all 3 Knots in Program GO-15352. The previous COS observations show that the fluxes are not high enough to warrant turning off Segment A for any of our targets in any of our spectroscopic exposures. Target acquisition time is based on existing COS/NUV acquisition images of Haro 11 taken with MIRRORA for GO-15352. Based on the observed flux in Knot C, acquisition exposure time of 10 sec yields S/N of 40. For the other knots, we will use Knot C for the target acquisition and offset the pointing accordingly. Knot A is an extended group of smaller clusters, so we set the ORIENT to minimize contamination. Knot B similarly has some extended emission, and also has ORIENT limits.
We also will obtain imaging with 1 orbit using WFC3 in filter FQ492N to capture H-beta. We take exposures dithered at 3 POS-TARGs to improve spatial resolution and mitigate cosmic rays. We also request a POST-FLASH to attain a 20 e background as recommended to mitigate the CTE issues.The entire team has extensive expertise with local candidate LCEs and LAEs and most have worked directly on Haro 11 in particular. PI Oey, along with Jaskot, has done extensive work on Green Pea galaxies (e.g., Jaskot & Oey 2013, 2014; Jaskot+ 2017, 2019). Jaskot is leading the HST Large program, "The Low-Redshift Lyman Continuum Survey" to obtain COS LyC observations in a variety of low-redshift LCE candidates (GO-15626). Both also previously worked on Haro 11 LyC in collaboration with then-undergraduate Ryan Keenan (Keenan, Oey, Jaskot+ 2017), and they are leading proponents exploring the suppressed superwind model for extreme feedback in LCEs (e.g., Gray, Oey+ 2019, Oey+ 2019; Jaskot+19; Oey+ 2017). Oey has also worked on X-ray emission from LAEs (Dittenber, Oey... Hayes, Oestlin+ 2020).
Leitherer and Hernandez have detailed expertise with optimizing COS observations at the LyC to evaluate the presence of emission in LCE candidates (e.g., Hernandez, Leitherer+ 2018; Leitherer, Hernandez, Lee, & Oey 2016; Borthakur, Heckman, Leitherer+ 2014). Hernandez is leading AR-15799, described in the text, to develop a new pipeline that optimizes dark current calibration.
Oestlin and his team have extensive expertise with local LAEs and LCEs, and Haro 11 in particular (e.g., Oestlin+ 2015, 2014, 2009). He is leading GO-15352 obtaining COS and STIS spectroscopy of Haro 11 at longer wavelengths to study the radiative transfer. Adamo, Bik, Hayes, Kunth, Laursen, Mas-Hesse, Oey, and Rivera-Thorsen are all Co-Is on this work. Adamo has expertise on SSC SED modeling, including Haro 11 (e.g., Adamo+ 2010, 2017); Bik has expertise with LyC radiative transfer in a similar LCE, ESO 338-IG04 (e.g., Bik+ 2018, 2015); Hayes is an expert on Lya radiative transfer and its relation to LyC, including in Haro 11 (e.g., Hayes+ 2007, 2010, 2013); Kunth is a pioneer of Lya radiative transfer and blue compact galaxies (e.g., Kunth & Oestlin 2000; Kunth 1995); Laursen is an expert on cosmological Lya radiative transfer (e.g., Laursen+ 2019, 2013); Mas-Hesse is an expert on starbursts and LAEs, including their X-ray sources (e.g., Oti-Floranes, Mas-Hesse+ 2012, 2014); Rivera-Thorsen has expertise on LCEs and LAEs both locally, including Haro 11, and at moderate redshift (e.g., Rivera-Thorsen+ 2017, 2019).Galaxies6falsefalsetruefalsefalsefalsefalseSUPPORTEDEXT-CLUSTEREMISSION LINE NEBULAKNOTNUCLEUSSTAR FORMING REGIONNOV-mag = HRC/F550M. Magnitudes obtained with 1 arcsec radius aperture.
FUV=1.93E-14 erg/s/cm2 at 1530 A, within 1.25 arcsec radius COS aperture, measured from ACS/SBC F140LP.
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:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "31"
:si-bright-earth-limb-angle 20.0
:data-volume 34944
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16260
:visit-id "15"
:obset-id "15"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16260
:visit-id "15"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2786
:al-overhead-at-end 0
:internal-dur-at-end 331
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3180
:pcs-gap 0
)true10Exposure time based on existing COS acquisition of this object.The scheduling data was generated by CASM 29.0.CASM was run in Phase II mode.Multiple previous COS observations for GO-15352 use Knot C for target acquisition. These observations show that the fluxes are not high enough to warrant turning off Segment A for any of our targets in any of our spectroscopic exposures. Target acquisition time is based on existing COS/NUV acquisition images of Haro 11 taken with MIRRORA for GO-15352. Based on the observed flux in Knot C, acquisition exposure time of 10 sec yields S/N of 40.1653065858000223.0(Tic-Visit
:proposal-id 16260
:visit-id "07"
:proposal-version -1
:trans-version "20200619"
:date "27-May-2021 10:59:12.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "31"
:si-bright-earth-limb-angle 20.0
:data-volume 52416
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16260
:visit-id "07"
:obset-id "07"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16260
:visit-id "07"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2786
:al-overhead-at-end 0
:internal-dur-at-end 38
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3180
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16260
:visit-id "07"
:orbit-number 2
:pcs-time 392
:si-vis-utilization 2787
:al-overhead-at-end 0
:internal-dur-at-end 331
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3180
:pcs-gap 0
)true20Exposure time based on existing COS acquisition of this object.The scheduling data was generated by CASM 30.1.CASM was run in Phase II mode.(Tic-Visit
:proposal-id 16260
:visit-id "08"
:proposal-version -1
:trans-version "20211222"
:date "11-May-2022 14:12:13.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "31"
:si-bright-earth-limb-angle 20.0
:data-volume 52416
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16260
:visit-id "08"
:obset-id "08"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16260
:visit-id "08"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2680
:al-overhead-at-end 0
:internal-dur-at-end 38
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3074
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16260
:visit-id "08"
:orbit-number 2
:pcs-time 392
:si-vis-utilization 2681
:al-overhead-at-end 0
:internal-dur-at-end 334
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3074
:pcs-gap 0
)false20Exposure time based on existing COS acquisition of this object.The scheduling data was generated by CASM 30.1.CASM was run in Phase II mode.(Tic-Visit
:proposal-id 16260
:visit-id "09"
:proposal-version -1
:trans-version "20211222"
:date "11-May-2022 14:12:54.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 2
:saa-model "31"
:si-bright-earth-limb-angle 20.0
:data-volume 52416
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16260
:visit-id "09"
:obset-id "09"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16260
:visit-id "09"
:orbit-number 1
:pcs-time 393
:si-vis-utilization 2680
:al-overhead-at-end 0
:internal-dur-at-end 38
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3074
:pcs-gap 0
)
(Tic-Orbit
:proposal-id 16260
:visit-id "09"
:orbit-number 2
:pcs-time 392
:si-vis-utilization 2681
:al-overhead-at-end 0
:internal-dur-at-end 334
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3074
:pcs-gap 0
)false20Exposure time based on existing COS acquisition of this object.The scheduling data was generated by CASM 29.0.CASM was run in Phase II mode.POS-TARG is applied for manual dithering to improve the spatial resolution.161154667400088.35905562703078(Tic-Visit
:proposal-id 16260
:visit-id "10"
:proposal-version -1
:trans-version "20200619"
:date "27-May-2021 10:59:14.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 211168
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16260
:visit-id "10"
:obset-id "10"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16260
:visit-id "10"
:orbit-number 1
:pcs-time 383
:si-vis-utilization 2797
:al-overhead-at-end 175
:internal-dur-at-end 267
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3180
:pcs-gap 0
)true10