0Assigned ID: 4259
----- Attempting Submission 1 (Wed May 24 05:23:17 GMT 2023) -----
HST Phase I Proposal 4259 successfully submitted.
Receipt: # 4259-1
----- Attempting Submission 2 (Wed May 24 21:10:32 GMT 2023) -----
HST Phase I Proposal 4259 successfully submitted.
Receipt: # 4259-2The number of orbits used exceeds the number allocated
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
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.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
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.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
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.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
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.14 September 2023
First submission with strategy detailed in the Proposal Description section.
Any future revisions will be summarized here.
28 September 2023
Second submission with 60 seconds cut from each orbit to help facilitate earlier scheduling.
22 November 2023
Third submission with BUFFER-TIME values properly set to 2/3 * Buffer Fill Time from ETC calculations for science exposures.
Concern had been raised regarding IMAGE/ACQ exposure times, as ETC calculations are set for an extended target (2.5 arcsec source diameter),
while flux re-normalization assumes a point source (g = 19.0 --> 19.0 mag/sq arcsec).
My original ETC calculations (COS.ta.1888782) were based off of PID 15986 (PI: Brunker) and, e.g., COS.ta.1368726, which used this same strategy.
This program's PC suggests that, since our source is not likely smooth and uniformly filling the aperture,
the exposure time of the IMAGE/ACQ is likely fine as-is.
No changes have been made thus far, but it may be good to double check that this strategy employed will work out okay!
NOTE: Visit Planner was hanging, so I am submitting without it having completed (as per recommendation of the CS),
with expectation that, since the program is effectively unchanged, it should be able to be run by the PC just fine.
1 July 2024
Fourth submission with reduced exposure times due to reduce gyro mode reductions in usable orbital visibility.
BUFFER-TIME values have been revised to account for new ETC runs for each observation.
See "Proposal Description" for details.
21 January 2025
Fifth submission after HOPR requests for failed Visits 01 and 02.
Visit 03 will encompass a re-observation of G130M/1291 FP-POS = 3,4 (Orbit 1) and G140L/800 FP-POS = 4 (Orbit 2).
We required a revision of the partially failed Visit 01.
The first orbit will also require a re-acquisition, before splitting the remaining time between the two G130M/1291 FP-POS values.
Visit 04 will encompass a re-observation of G140L/800 FP-POS = 1,2,3,4.
It is a direct repeat of the original failed Visit 02.
8 December 2025
Sixth resubmission after HOPR request for failed Visit 03 Orbit 1.
Visit 05 will encompass a re-observation of G130M/1291 FP-POS = 3,4 (Orbit 1).
The exposure times for these two G130M/1291 FP-POS positions has been reduced from 876 to 867 seconds.
Note that a new ETC run provided an updated value for the Buffer Fill Time,
which is reflected now in the APT file as a new BUFFER-TIME in the Optional Parameters.
This change allows the requested re-observations to fit within the single orbit allocation.
The Visit 03 Orbit 2 (G140L/800 FP-POS = 4) completed successfully and will not be repeated.
Visit 04 has yet to execute and so is left as is.
8 January 2026
Seventh resubmission after HOPR request for failed Visit 05 Orbit 1.
Visit 06 will encompass a re-observation of G130M/1291 FP-POS = 3,4 (Orbit 1).23430116----- Attempting Submission 1 (Thu Sep 14 18:29:20 GMT 2023) -----
HST Phase II Proposal 17490 successfully submitted.
Receipt: # 17490-1
----- Attempting Submission 2 (Thu Sep 28 20:26:37 GMT 2023) -----
HST Phase II Proposal 17490 successfully submitted.
Receipt: # 17490-2
----- Attempting Submission 3 (Wed Nov 22 19:25:25 GMT 2023) -----
----- Attempting Submission 4 (Mon Jul 01 19:01:14 GMT 2024) -----
----- Attempting Submission 5 (Tue Jan 21 22:01:01 GMT 2025) -----
----- Attempting Submission 6 (Tue Dec 09 21:54:10 GMT 2025) -----
----- Attempting Submission 7 (Thu Jan 08 18:03:39 GMT 2026) -----These warnings all pertain to the fact that we are observing an extended target with COS, which we are aware of and should pose no problem.A Local Lyman Continuum Leaker: Direct and Indirect Detections with KISSB 85The specific mechanisms responsible for the reionization of the Universe remain poorly understood. While it is generally accepted that this period of transformation was primarily a consequence of highly-ionizing Lyman continuum (LyC) radiation leaking from high-redshift star-forming galaxies (SFGs), their direct detection is observationally precluded due to the high opacities of the ubiquitous intergalactic medium. Local analogs to these systems, with attributes which mirror the environments of the early Universe such as high ionization and low metal abundances, represent our best accessible means to obtain detailed measurements of LyC photons. We propose for COS far-ultraviolet (FUV) observations of the candidate LyC leaker KISSB 85, a nearby (z = 0.046; D = 206 Mpc), metal-poor (12+log(O/H) = 7.42; ~5% Z_solar), high-ionization (O32 = 17.3) SFG. This dwarf system possesses similar charateristics to early-Universe LyC leakers, but is nearby enough to allow for meticulous examination of its radiation profile. In addition, we will utilize these direct detections to examine an indirect means for estimating LyC with the saturated C II 1334.5 A absorption feature, which will allow for a broader understanding of the mechanisms which enable LyC leakage. With measurement of the Lyman-alpha line profile, we will study the neutral gas properties of this high-z analog system, and through efforts fitting the spectral profile with two different theoretical models, we will characterize the metallicity, age, and dust attenuation of the observed young, massive stellar population which produces the ionizing radiation, supporting current efforts being undertaken with JWST.We are observing the Lyman continuum (LyC) leaker candidate KISSB 85. This is a nearby (z = 0.046; D = 206 Mpc), metal-poor (12+log(O/H) = 7.42; ~5% Z_solar), high-ionization (O32 = 17.3) star-forming galaxy. Observations will be undertaken utilizing HST/COS far-ultraviolet (far-UV) spectroscopy with the G140L grating and cenwave 800, which will recover LyC photons (lambda_observed < 954.3 A) directly. Additionally, we will observe with HST/COS grating G130M and cenwave 1291, which will detect Lyman-alpha (Lya) photons (lambda_observed = 1272.0 A), as well as the C II 1334.5 A spectral feature (lambda_observed = 1396.4 A), which has proven a reliable proxy for measuring the LyC escape fraction when direct observations are precluded. This will enable us to better understand the mechanism(s) facilitating the escape of ionizing photons which are capable of ionizing the early Universe in the nearby, high-redshift star-forning galaxy analog KISSB 85. In addition, we will characterize Lya itself and, employing the near-UV target acquisition images, we will study the morphology of this compact system as well.
The exposure time necessary to acquire an ACQ/IMAGE with S/N = 20 was preliminarily calculated by the exposure time calculator (ETC) to be 219.25 seconds, which is much less than one orbit. G140L/800 spectroscopy of LyC photons with S/N = 2-3 was computed with the ETC to take 21,353.86 seconds, or approximately 6.7 orbits. G130M/1291 spectroscopy of Lya emission (S/N = 20) and the indirect C II feature (S/N >5) was computed with the ETC to take 3,429.93 seconds, or approximately 1.0 orbits. The total exposure time is estimated to require eight orbits.
Our observing strategy will be to split our eight orbits into two separate visits, as scheduling is limited to five orbits at a time, avoiding visits of four orbits, whenever possible. We therefore will conduct a first visit of five orbits, which will begin with an imaging acquisition. The remainder of this first orbit will then be taken up entirely with an exposure of G140L/800 at FP-POS = 1. The subsequent three orbits (orbits 2, 3, and 4 of visit 1) will each be entirely comprised of G140L/800 exposures, at FP-POS = 2, 3, and 4, respectively. Finally, the last orbit of this visit (orbit 5) will be split between the two allowed G130M/1291 FP-POS settings (3 and 4).
The second visit will then be three orbits, which will again begin with an imaging acquisition. Once again, the remainder of this first orbit will be entirely taken up with an exposure of G140L/800 at FP-POS = 1. Orbit 2 will be split evenly between G140L/800 FP-POS = 2 and 3. Finally, the last orbit of the visit (orbit 3) will be entirely dedicated to G140L/800 FP-POS = 4.
This strategy results in uneven exposure times for the four FP-POS settings of G140L/800, with emphasis on FP-POS = 4. This is because, of the four FP-POS possible, FP-POS = 4 goes to the shortest wavelength, which will give us the best possible chance at recovering LyC photons. The total exposure time for each of the four G140L/800 FP-POS settings are as follows:
FP-POS First Integration Second Integration Total Exposure Time
---------------------------------------------------------------
1 1909 seconds 1909 seconds 3818 seconds
2 2688 seconds 1286 seconds 3974 seconds
3 2688 seconds 1286 seconds 3974 seconds
4 2688 seconds 2688 seconds 5376 seconds
---------------------------------------------------------------
We note that, comparing the ETC computations made for this APT Phase II file with those made for the initial Phase I submission in May 2023, there had been a version update of pyETC (v31.1 to v31.2) within which the dark rates (as reported via monitoring by the HST/COS Instrument Team) were elevated significantly. This has the effect of requiring a longer science integration time to achieve the same S/N. Due to the necessities of the strategy outlined here, including time lost to overheads, the number of orbits which will be dedicated to G140L/800 (~6.5) is a bit less than proposed for (~6.7). This has the consequence of potentially lowering the S/N expected for LyC photons, however as we expect to bin heavily below the Lyman Break in effort to recover said photons, this should not be a problem.
Here now is a summary of the observing program strategy:
Visit Orbit Mode FP-POS Exp. Time ETC#
--------------------------------------------------------------------
1 1 IMAGE/ACQ N/A 221 sec COS.ta.1888782
1 1 G140L/800 1 1909 sec COS.sp.1888785
1 2 G140L/800 2 2686 sec COS.sp.1888786
1 3 G140L/800 3 2686 sec COS.sp.1888786
1 4 G140L/800 4 2686 sec COS.sp.1888786
1 5 G130M/1291 3 1285 sec COS.sp.1888783
1 5 G130M/1291 4 1285 sec COS.sp.1888783
2 1 IMAGE/ACQ N/A 221 sec COS.ta.1888782
2 1 G140L/800 1 1909 sec COS.sp.1888785
2 2 G140L/800 2 1286 sec COS.sp.1888784
2 2 G140L/800 3 1286 sec COS.sp.1888784
2 3 G140L/800 4 2686 sec COS.sp.1888786
--------------------------------------------------------------------
BUFFER-TIME values for science exposures were set to be 2/3 * Buffer Fill Time reported in the ETC calculations. For the G140L/800 observations, 10,101 sec * 2/3 = 6,734 sec. For the G130M/1291 observations, 5,883 sec * 2/3 = 3,922 sec.
UPDATE (1 July 2024): Due to HST now operating under reduced gyro mode (RGM), the usable exposure duration per orbit has been reduced further. In addition, at this point in time the ETC version has been updated to 32.2. Here are updated records for the ETC runs, where the BUFFER-TIME has been revised to reflect the constraints of the exposure times.
(G140L/800)
FP-POS First Integration Second Integration Total Exposure Time
---------------------------------------------------------------
1 1860 seconds 1860 seconds 3720 seconds
2 2588 seconds 1236 seconds 3824 seconds
3 2588 seconds 1237 seconds 3825 seconds
4 2588 seconds 2588 seconds 5176 seconds
---------------------------------------------------------------
(observing program summary)
Visit Orbit Mode FP-POS Exp. Time ETC#
--------------------------------------------------------------------
1 1 IMAGE/ACQ N/A 221 sec COS.ta.1888782
1 1 G140L/800 1 1860 sec COS.sp.1926681
1 2 G140L/800 2 2588 sec COS.sp.1926380
1 3 G140L/800 3 2588 sec COS.sp.1926380
1 4 G140L/800 4 2588 sec COS.sp.1926380
1 5 G130M/1291 3 1216 sec COS.sp.1926381
1 5 G130M/1291 4 1217 sec COS.sp.1926381
2 1 IMAGE/ACQ N/A 221 sec COS.ta.1888782
2 1 G140L/800 1 1860 sec COS.sp.1926681
2 2 G140L/800 2 1236 sec COS.sp.1926678
2 2 G140L/800 3 1237 sec COS.sp.1926678
2 3 G140L/800 4 2588 sec COS.sp.1926380
--------------------------------------------------------------------
UPDATE (21 January 2025): Due to failed observations for both Visit 01 (partial) and 02 (complete), I have had to revise the APT file. In short, the first three Orbits for Visit 01 executed successfully, but the final two Orbits failed. My repeat for Visit 01 (which will be Visit 03) will therefore consist of one Orbit consisting of an imaging target acquisition, then FP-POS = 3 and 4 of G130M/1291, followed by a second Orbit consisting entirely of G140L/800 FP-POS = 4. The repeat for Visit 02 (which will be Visit 04) is simply a like for like repeat.
By squeezing the IMAGE/ACQ with the two G130M/1291 FP-POS settings into one orbit, I've had to reduce the observing time for the science exposures, in effort to keep the G140L/800 observation integrating as long as possible.
(observing program summary)
Visit Orbit Mode FP-POS Exp. Time ETC#
--------------------------------------------------------------------
3 1 IMAGE/ACQ N/A 221 sec COS.ta.1888782
3 1 G130M/1291 3 876 sec COS.sp.1947976
3 1 G130M/1291 4 876 sec COS.sp.1947976
3 2 G140L/800 4 2588 sec COS.sp.1926380
4 1 IMAGE/ACQ N/A 221 sec COS.ta.1888782
4 1 G140L/800 1 1860 sec COS.sp.1926681
4 2 G140L/800 2 1236 sec COS.sp.1926678
4 2 G140L/800 3 1237 sec COS.sp.1926678
4 3 G140L/800 4 2588 sec COS.sp.1926380
--------------------------------------------------------------------
UPDATE (8 December 2025): Due to a failed observation for Visit 03, I am revising the APT file. In short, it appears that, of the two Orbits for Visit 03, Orbit one (IMAGE/ACQ, then G130M/1291 FP-POS = 3 and 4) failed, but Orbit two (G140L/800) succeeded. Svea submitted a HOPR request to re-do the failed Orbit, which was approved, so I am going to have a new Visit 05 that consists only of the IMAGE/ACQ and G130M/1291 FP-POS = 3 and 4 exposures. This will simply be a like for like repeat of Visit 03 Orbit one, since G140L/800 (Orbit two) was unaffected. The Visit 04 has yet to happen, so I will leave that as is.
Because the length of orbital visibility has apparently decreased slightly since the last time I re-submitted this program, a small amount of time had to shaved off from each of the G130M/1291 exposures in order for the proposed observations to fit within a single orbit, and maintaining the IMAGE/ACQ exposure duration. As a consequence, the G130M/1291 FP-POS = 3 and 4 exposure times have been reduced from 876 to 867 seconds each. These changes have been documented with a new ETC simulation in the Table below. There is consequently a slightly reduced expected S/N for these exposures.
(observing program summary)
Visit Orbit Mode FP-POS Exp. Time ETC#
--------------------------------------------------------------------
4 1 IMAGE/ACQ N/A 221 sec COS.ta.1888782
4 1 G140L/800 1 1860 sec COS.sp.1926681
4 2 G140L/800 2 1236 sec COS.sp.1926678
4 2 G140L/800 3 1237 sec COS.sp.1926678
4 3 G140L/800 4 2588 sec COS.sp.1926380
5 1 IMAGE/ACQ N/A 221 sec COS.ta.1888782
5 1 G130M/1291 3 867 sec COS.sp.2260162
5 1 G130M/1291 4 867 sec COS.sp.2260162
--------------------------------------------------------------------
UPDATE (8 January 2026): Due to a failed observation for Visit 05, I am revising the APT file. In short, it appears that, for the single Orbit for Visit 05, the G130M/1291 FP-POS = 3 and 4 observations failed. I submitted a HOPR request which was approved, so I am going to have a new Visit 06 that consists only of the IMAGE/ACQ and G130/1291 FP-POS = 3 and 4 exposures. This will simply be a like for like repeat of Visit 05. Since the last time I had to revise the APT file was very recently, none of the observing parameters have changed, and so the program summary is in the Table below.
(observing program summary)
Visit Orbit Mode FP-POS Exp. Time ETC#
--------------------------------------------------------------------
6 1 IMAGE/ACQ N/A 221 sec COS.ta.1888782
6 1 G130M/1291 3 867 sec COS.sp.2260162
6 1 G130M/1291 4 867 sec COS.sp.2260162
--------------------------------------------------------------------Dr. Alec Hirschauer is an expert in the analysis and interpretation of emission-line spectra of low-mass star-forming galaxies as local analogs to high-redshift systems. He is a member of the HST/COS instrument team and has expertise in its use and capabilities. He will lead the science analysis and manage the contribution of the Co-Is.
Dr. Samantha Brunker is an expert on compact, extreme star-forming galaxies, and has previously led a successful HST/COS program studying Lyman continuum leakers using similar methods as those proposed here.
Dr. John Salzer is an expert in the analysis and interpretation of emission-line spectra of low-mass star-forming galaxies as local analogs to high-redshift systems. He is the PI of the KPNO International Spectroscopic Survey, from which the target (KISSB 85) was originally discovered.
Dr. Svea Hernandez is an expert on the chemical abundances of star clusters and the interstellar medium, which is used to understand the chemical histories of galaxies at different times. She has previously led a successful HST/COS program studying Lyman continuum leaking galaxies, with special emphasis on using the CII feature as an indirect tracer. She is a member of the HST/COS instrument team and has expertise with data reduction and analysis of FUV data.
Dr. Bethan James has ample experience with HST/COS and is a former deputy manager of the instrument team. She has lead several HST/COS observing campaigns to study environments of nearby star-forming galaxies, and is an expert in the derivation of chemical abundances of star-forming galaxies using both UV and optical spectroscopy.
Dr. Alessandra Aloisi has expertise in the analysis of spectroscopic observations to obtain column densities and chemical abundances of both the gas and stellar components in extragalactic environments. She has particular technical expertise in UV spectroscopy with space-based telescopes, having led the COS+STIS instrument team for several years, acquiring knowledge on the strengths and weaknesses of the spectrographs.
Dr. Matilde Mingozzi is an expert in interstellar medium properties (including outflows, gas-phase abundances, etc.), with ample experience analyzing COS spectroscopic observations of star-forming galaxies.
Dr. Logan Jones has extensive experience with Lyman continuum studies at high redshifts (z ~ 3), having lead several different projects and publications searching for Lyman continuum candidates. He is also an expert in the analysis of COS observations.
Dr. Claus Leitherer is an expert in Lyman continuum studies, with research focuses in properties of individual massive stars and of young stellar populations, population synthesis modeling, spectral energy distributions of galaxies, and ultraviolet to near-infrared observations of galaxies.
Dr. Swara Ravindranath is an expert on spectroscopic studies of extreme emission-line galaxies and has used HST/COS and STIS to study local analogs of high redshift star forming galaxies. She uses photoionization models to understand the conditions for strong nebular emission and to infer the ionizing spectra of low-metallicity star forming galaxies.GalaxiesStellar Populations and the Interstellar Medium6falsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTEMISSION LINE NEBULASTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.
See http://ned.ipac.caltech.edu/byname?objname=KISSB+85&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1 for more "Other Fluxes".J2000J2000m_B = 19.85, FUV (GALEX) AB = 20.1377 +/- 0.1793, g (SDSS model) AB = 19.016 +/- 0.013COS/FUVSpectroscopicNoNoG130M1291COS/FUVSpectroscopicNoNoG140L800The scheduling data was generated by CASM 34.0.CASM was run in Phase II mode./private/var/folders/bx/4nynjn_s397fm2_wr4k1mk740000gn/T/OPVisit5096575082695070552.xml1731398018000310.8174511445744(Tic-Visit
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)true55Original BUFFER-TIME = 10101 seconds (from ETC's Buffer Fill Time) * 2/3 = 6734 seconds
New BUFFER-TIME = 11709 seconds (from ETC's Buffer Fill Time) * 2/3 = 7806 secondsOriginal BUFFER-TIME = 10101 seconds (from ETC's Buffer Fill Time) * 2/3 = 6734 seconds
New BUFFER-TIME = 10939 seconds (from ETC's Buffer Fill Time) * 2/3 = 7293 secondsOriginal BUFFER-TIME = 10101 seconds (from ETC's Buffer Fill Time) * 2/3 = 6734 seconds
New BUFFER-TIME = 10939 seconds (from ETC's Buffer Fill Time) * 2/3 = 7293 secondsOriginal BUFFER-TIME = 10101 seconds (from ETC's Buffer Fill Time) * 2/3 = 6734 seconds
New BUFFER-TIME = 10939 seconds (from ETC's Buffer Fill Time) * 2/3 = 7293 secondsOriginal BUFFER-TIME = 5883 seconds (from ETC's Buffer Fill Time) * 2/3 = 3922 seconds
New BUFFER-TIME = 6418 seconds (from ETC's Buffer Fill Time) * 2/3 = 4279 secondsOriginal BUFFER-TIME = 5883 seconds (from ETC's Buffer Fill Time) * 2/3 = 3922 seconds
New BUFFER-TIME = 6418 seconds (from ETC's Buffer Fill Time) * 2/3 = 4279 secondsThe scheduling data was generated by CASM 34.0.CASM was run in Phase II mode./private/var/folders/bx/4nynjn_s397fm2_wr4k1mk740000gn/T/OPVisit15994947965207641351.xml1734281018000303.26904537218707(Tic-Visit
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New BUFFER-TIME = 11709 seconds (from ETC's Buffer Fill Time) * 2/3 = 7806 secondsOriginal BUFFER-TIME = 10101 seconds (from ETC's Buffer Fill Time) * 2/3 = 6734 seconds
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