Date: October 3rd 2010

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Daily Report #5192 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/56ac452e4618e5da?hl=en
Daily Report #5193 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/5d666ade893ac663?hl=en

============================================================================== TOPIC: Daily Report #5192

http://groups google com/group/sci astro hubble/t/56ac452e4618e5da?hl=en

== 1 of 1 == Date: Thurs, Sep 30 2010 9:26Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5192

PERIOD COVERED: 8pm September 28 - 7:59pm September 29, 2010 (DOY 272/00:00z-272/23:59z)

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated )

HSTARS:

12436 - OBAD at 272/01:25z, GSAcq(2,1,1) at 272/01:32z and REAcq at 272/02:44:05z all failed with Search Radius Limit exceeded on FGS2

Observations affected: ACS 35-38, Proposal ID#12381

HSTAR FOR DOY 261

12439 - REAcq(1,2,1) at 261/01:32:50z received a stop flag on FGS1 three times before achieving FL-DV The acquisition was successful

Observations possibly affected: COS 41-46 Proposal ID#11896; STIS 95-97 Proposal ID#11847

COMPLETED OPS REQUEST: (None)

COMPLETED OPS NOTES: (None)

                    Scheduled  Successful

FGS GSAcq 8 7 FGS REAcq 8 7 OBAD with Maneuver 7 7

SIGNIFICANT EVENTS: (None)

OBSERVATIONS SCHEDULED:

ACS/WFC 11996

CCD Daily Monitor (Part 3)

This program comprises basic tests for measuring the read noise and dark current of the ACS WFC and for tracking the growth of hot pixels The recorded frames are used to create bias and dark reference images for science data reduction and calibration This program will be executed four days per week (Mon, Wed, Fri, Sun) for the duration of Cycle 17 To facilitate scheduling, this program is split into three proposals This proposal covers 308 orbits (19 25 weeks) from 21 June 2010 to 1 November 2010

ACS/WFC 12210

SLACS for the Masses: Extending Strong Lensing to Lower Masses and Smaller Radii

Strong gravitational lensing provides the most accurate possible measurement of mass in the central regions of early-type galaxies (ETGs) We propose to continue the highly productive Sloan Lens ACS (SLACS) Survey for strong gravitational lens galaxies by observing a substantial fraction of 135 new ETG gravitational-lens candidates with HST-ACS WFC F814W Snapshot imaging The proposed target sample has been selected from the seventh and final data release of the Sloan Digital Sky Survey, and is designed to complement the distribution of previously confirmed SLACS lenses in lens-galaxy mass and in the ratio of Einstein radius to optical half-light radius The observations we propose will lead to a combined SLACS sample covering nearly two decades in mass, with dense mapping of enclosed mass as a function of radius out to the half-light radius and beyond With this longer mass baseline, we will extend our lensing and dynamical analysis of the mass structure and scaling relations of ETGs to galaxies of significantly lower mass, and directly test for a transition in structural and dark-matter content trends at intermediate galaxy mass The broader mass coverage will also enable us to make a direct connection to the structure of well-studied nearby ETGs as deduced from dynamical modeling of their line-of-sight velocity distribution fields Finally, the combined sample will allow a more conclusive test of the current SLACS result that the intrinsic scatter in ETG mass-density structure is not significantly correlated with any other galaxy observables The final SLACS sample at the conclusion of this program will comprise approximately 130 lenses with known foreground and background redshifts, and is likely to be the largest confirmed sample of strong-lens galaxies for many years to come

ACS/WFC 12381

Lmaging the Crab Nebula while it is Flaring in Gamma-rays

The high energy gamma-ray flux from the Crab nebula doubled in a couple of days (from September 19 to September 21) Such enhancement, never seen before, is clearly detected both by Agile and Fermi, the two gamma-ray telescopes currently in operation While such huge brightening is exciting the entire astrophysical community, TOOs are being scheduled by high energy space observatories such as Integral, Swift and Chandra By imaging the status of the knots and wisps in the inner Crab nebula, HST could provide a unique piece of information, which may yield a clue to understand the source behavior

ACS/WFC/WFC3/UV 12213

The Stellar Halo Profiles of Massive Disk Galaxies

Stellar halos surrounding massive galaxies are of prime interest in hierarchical galaxy formation models: most of the halo is formed by the very early accretion of small, metal poor satellite galaxies each with their independent evolution history As such, halos contain the fossil remnants of the earliest star formation and accretion phases of a galaxy in formation The resulting size, shape, age, and metallicity of stellar halos provide therefore a direct test of the basic ingredients (reionization, feedback from star formation, density fluctuation power spectrum) of hierarchical galaxy formation models

In our GHOSTS survey we have sampled the principle axes of a sample of 11 nearby galaxies with Vrot>100 km/s Our detection of resolved stellar halo populations ~1 5 mag below the tip of the Red Giant Branch has revealed halos that extend as far as 30 kpc around the most massive galaxies in our sample Those extended stellar halos seem more compact than current model predictions, they have unexpectedly high metallicity up to the last detected point, and have a luminosity that is more closely related to the bulge luminosity than to the galaxy mass We propose to extend the light profiles of 4 massive galaxies with a range in bulge-to-disk ratio to the background limit at ~70 kpc This will enable us to:

confirm the stellar halo shape (compactness) and assess with confidence any conflict with models using these very extended and accurate halo profile characterizations;
establish whether stellar envelopes beyond 30 kpc are still morphologically connected to inner bulges, or whether a break occurs at larger radii revealing a distinct new component;
determine whether every massive galaxy has an old, metal-poor halo at large radius like the Milky Way and M31; if not, constrain for the first time the range of stellar metallicity gradients in extended stellar halos

COS/NUV 12041

COS-GTO: Io Atmosphere/STIS

We will use six HST orbits with COS to observe the disk-integrated longitudinal distribution of Io's atmosphere, and ten HST orbits with STIS to provide complementary disk-resolved information at key locations We will use the COS G225M grating to observe four SO2 absorption bands, which can be used to determine SO2 atmospheric density Disk-integrated 19 micron observations of the atmosphere indicate that the anti-Jupiter hemisphere of Io has an atmospheric density roughly ten times greater than the Jupiter-facing side (Spencer et al 2005), and mm-wave observations suggest a similar pattern However the infrared and mm-wave observations cannot easily separate atmospheric density from atmospheric temperature, so these results are model-dependent Sparse 2100 2300 disk-resolved observations (McGrath et al 2000, Jessup et al 2004) tell a consistent story, but do not cover enough of Io's surface to provide full confirmation of the long-wavelength result We will therefore observe Io's disk-integrated atmospheric density at six longitudes, roughly 30, 90, 150, 210, 270, and 330 W, to confirm the 19 micron results and improve our ability to model the 19-micron data With STIS, we plan disk-resolved 2000-3200 spectroscopy of Io's SO2 atmosphere Our observations will target low-latitude regions away from active plumes (in contrast to our Cycle 10 observations (Jessup et al 2004) which targeted the Prometheus plume), to look for the effect of plumes on the atmosphere We will also look at the variation of low-latitude atmospheric abundance with terrain type, to look for explanations for the large longitudinal variations in atmospheric pressure to be studied with COS Finally, we will look at a variety of regions at two different times of day to determine the extent of diurnal variations in the atmosphere, which are expected if the atmosphere is dominantly supported by frost sublimation

STIS/CCD 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD

STIS/CCD 11847

CCD Bias Monitor-Part 2

Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns

WFC3/IR 11926

IR Zero Points

We will measure and monitor the zeropoints through the IR filters using observations of the white dwarf standard stars, GD153, GD71 and GD191B2B and the solar analog standard star, P330E Data will be taken monthly during Cycle 17 Observations of the star cluster, NGC 104, are made twice to check color transformations We expect an accuracy of 2% in the wide filter zeropoints relative to the HST photometric system, and 5% in the medium- and narrow-band filters

WFC3/IR 12181

The Atmospheric Structure of Giant Hot Exoplanets

Characterization of close-in giant exoplanets has proceeded rapidly over the past few years, due largely to Spitzer and HST observations in transiting systems Low resolution thermal emission spectra of over two dozen planets have been measured by Spitzer, and HST observations of a few key planets have indicated unusual molecular abundances via transmission spectroscopy However, current models for the atmospheric structure of these worlds exhibit degeneracies wherein different combinations of temperature and molecular abundance profiles can fit the same Spitzer data for each planet Fortunately, the advent of the IR capability on HST/WFC3 allows us to solve this major problem in exoplanet science We propose to inaugurate a Large HST program that is scientifically complementary to Spitzer, Kepler, and CoRoT exoplanet results

We will obtain transmission spectroscopy of the 1 4-micron water band in a sample of 13 planets, using the G141 grism on WFC3 Among the abundant molecules, only water absorbs at this wavelength, and our measurement of water abundance will enable us to break the degeneracies in the Spitzer results with minimal model assumptions We will also use the G141 grism to observe secondary eclipses for 7 very hot giant exoplanets at 1 5-microns, including several bright systems in the Kepler and CoRoT fields The strong temperature sensitivity of the thermal continuum at 1 5-microns provides high leverage on atmospheric temperature for these worlds, again helping to break degeneracies in interpreting the Spitzer data Moreover, our precise eclipse photometry, in combination with extant Spitzer data, will enable us to extrapolate the thermal continuum to optical wavelengths Kepler and CoRoT teams will be thereby able to subtract the thermal contribution from their increasingly precise measurements of optical eclipses, and measure, or place extremely stringent limits on, the albedo of these exotic worlds

WFC3/UV 12215

Searching for the Missing Low-Mass Companions of Massive Stars

Recent results on binary companions of massive O stars appear to indicate that the distribution of secondary masses is truncated at low masses It thus mimics the distribution of companions of G dwarfs and also the Initial Mass Function (IMF), except that it is shifted upward by a factor of 20 in mass These results, if correct, provide a distribution of mass ratios that hints at a strong constraint on the star-formation process However, this intriguing result is derived from a complex simulation of data which suffer from observational incompleteness at the low-mass end

We propose a snapshot survey to test this result in a very direct way HST WFC3 images of a sample of the nearest Cepheids (which were formerly B stars of ~5 Msun) will search for low-mass companions down to M dwarfs We will confirm any companions as young stars, and thus true physical companions, through follow-up Chandra X-ray images Our survey will show clearly whether the companion mass distribution is truncated at low masses, but at a mass much higher than that of the IMF or G dwarfs

WFC3/UV 12348

WFC3/UVIS Charge Injection Test

In preparation for making charge injection (CI) available to observers, this proposal will 1) confirm that the CI performs on-orbit as it did on the ground, 2) provide an initial assessment of which CI mode is most effective (10, 17, 25 line or continuous), and 3) obtain a baseline calibration for each mode

WFC3/UVIS 11729

Photometric Metallicity Calibration with WFC3 Specialty Filters

The community has chosen to include several filters in the WFC3 filter complement that have been designed to allow fairly precise estimates of stellar metallicities, and many science programs are enabled by this capability Since these filters do not exactly match those used for this purpose on the ground, however, the mapping of stellar colors to stellar metallicities needs to be calibrated We propose to achieve this calibration through observations of five stellar clusters with well known metallicities We will calibrate several different filter calibrations which will allow future users to determine what filter combination best meets their science needs

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

The behavior of the WFC3 UVIS CCD will be monitored daily with a set of full-frame, four-amp bias and dark frames A smaller set of 2Kx4K subarray biases are acquired at less frequent intervals throughout the cycle to support subarray science observations The internals from this proposal, along with those from the anneal procedure (Proposal 11909), will be used to generate the necessary superbias and superdark reference files for the calibration pipeline (CDBS)

WFC3/UVIS 11914

UVIS Earth Flats

This program is an experimental path finder for Cycle 18 calibration Visible-wavelength flat fields will be obtained by observing the dark side of the Earth during periods of full moon illumination The observations will consist of full-frame streaked WFC3 UVIS imagery: per 22- min total exposure time in a single "dark-sky" orbit, we anticipate collecting 7000 e/pix in F606W or 4500 e/pix in F814W To achieve Poisson S/N > 100 per pixel, we require at least 2 orbits of F606W and 3 orbits of F814W

For UVIS narrowband filters, exposures of 1 sec typically do not saturate on the sunlit Earth, so we will take sunlit Earth flats for three of the more-commonly used narrowband filters in Cycle 17 plus the also-popular long-wavelength quad filters, for which we get four filters at once

Why not use the Sunlit Earth for the wideband visible-light filters? It is too bright in the visible for WFC3 UVIS minimum exposure time of 0 5 sec Similarly, for NICMOS the sunlit-Earth is too bright which saturates the detector too quickly and/or induces abnormal behaviors such as super-shading (Gilmore 1998, NIC 098-011) In the narrowband visible and broadband near- UV its not too bright (predictions in Cox et al 1987 "Standard Astronomical Sources for HST: 6 Spatially Flat Fields " and observations in ACS Program 10050)

Other possibilities? Cox et al 's Section II D addresses many other possible sources for flat fields, rejecting them for a variety of reasons A remaining possibility would be the totally eclipsed moon Such eclipses provide approximately 2 hours (1 HST orbit) of opportunity per year, so they are too rare to be generically useful An advantage of the moon over the Earth is that the moon subtends less than 0 25 square degree, whereas the Earth subtends a steradian or more, so scattered light and light potentially leaking around the shutter presents additional problems for the Earth Also, we're unsure if HST can point 180 deg from the Sun

============================================================================== TOPIC: Daily Report #5193

http://groups google com/group/sci astro hubble/t/5d666ade893ac663?hl=en

== 1 of 1 == Date: Fri, Oct 1 2010 7:46Ã‚Â am From: "Cooper, Joe"

HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science

DAILY REPORT #5193

PERIOD COVERED: 8:00pm September 29 - 7:59pm September 30, 2010 (DOY 273/00:00z-273/23:59z)

FLIGHT OPERATIONS SUMMARY:

Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated )

HSTARS:

12441 - ACS Suspend at 273/11:51z

Observations affected: ACS #62-65, Proposal #11575

12442 - GSAcq(2,1,1) scheduled at 273/16:44:20z results in fine lock backup (2,0,2), scan step limit exceeded on FGS-2

Observations possibly affected: COS 95-100 Proposal ID#12041, WFC3 164 Proposal ID#12348

COMPLETED OPS REQUEST: 18931-2 - Dump ACS memory at 273/1312z 18932-1 - Recover ACS from Suspend Mode at 273/2103z

COMPLETED OPS NOTES: (None)

                    Scheduled   Successful

FGS GSAcq 8 8 FGS REAcq 7 7 OBAD with Maneuver 6 6

SIGNIFICANT EVENTS:

FLASH REPORT: ACS Suspended at 273/11:51z

FLASH REPORT: ACS Suspend Recovery Side 1 was successfully completed at 2010/273/21:03 UTC, returning ACS to its nominal WFHROper state in readiness to intercept the on-going science timeline

OBSERVATIONS SCHEDULED:

ACS/WFC/WFC3/UV 12213

The Stellar Halo Profiles of Massive Disk Galaxies

confirm the stellar halo shape (compactness) and assess with confidence any conflict with models using these very extended and accurate halo profile characterizations;
establish whether stellar envelopes beyond 30 kpc are still morphologically connected to inner bulges, or whether a break occurs at larger radii revealing a distinct new component;
determine whether every massive galaxy has an old, metal-poor halo at large radius like the Milky Way and M31; if not, constrain for the first time the range of stellar metallicity gradients in extended stellar halos

ACS/WFC3 11575

The Stellar Origins of Supernovae

Supernovae (SNe) have a profound effect on galaxies, and have been used recently as precise cosmological probes, resulting in the discovery of the accelerating Universe They are clearly very important events deserving of intense study Yet, even with nearly 4000 known SNe, we know relatively little about the stars which give rise to these powerful explosions The main limitation has been the lack of spatial resolution in pre-SN imaging data However, since 1999 our team has been at the vanguard of directly identifying SN progenitor stars in HST images From this exciting new line of study, the emerging trend from 5 detections for Type II- Plateau SNe is that their progenitors appear to be relatively low mass (8 to 20 Msun) red supergiants, although more cases are needed Nonetheless, the nature of the progenitors of Type Ib/c SNe, a subset of which are associated with the amazing gamma-ray bursts, remains ambiguous Furthermore, we remain in the continually embarrassing situation that we still do not yet know which progenitor systems explode as Type Ia SNe, which are currently being used for precision cosmology In Cycle 16 we have triggered on the Type Ic SN 2007gr and Type IIb SN 2008ax so far We propose to determine the identities of the progenitors of 4 SNe within 17 Mpc, which we expect to occur during Cycle 17, through ToO observations using ACS/HRC

COS/FUV 11526

COS-GTO: Sampling the Local ISM with Hot White Dwarfs

We shall use hot white dwarf stars located within 150pc of the Sun to probe the absorption properties of the interstellar gas associated with the local cavity There is still much debate concerning the ionization state of the local gas, since previously detected highly ionized lines (such as CIV and SiIV) could be associated with the circumstellar environments of hot white dwarfs By using a priori knowledge of the velocity structure of the interstellar sight-lines to these targets (gained from high spectral resolution ground-based observations) in conjunction with the UV absorption data gained with HST-COS, we shall be able to better determine both the physical and chemical state of the numerous diffuse interstellar clouds present within the local cavity

COS/NUV 12041

COS-GTO: Io Atmosphere/STIS

COS/NUV/FUV 11728

The Impact of Starbursts on the Gaseous Halos of Galaxies

Perhaps the most important (yet uncertain) aspects of galaxy evolution are the processes by which galaxies accrete gas and by which the resulting star formation and black hole growth affects this accreting gas It is believed that both the form of the accretion and the nature of the feedback change as a function of the galaxy mass At low mass the gas comes in cold and the feedback is provided by massive stars At high mass, the gas comes in hot, and the feedback is from an AGN The changeover occurs near the mass where the galaxy population transitions from star-forming galaxies to red and dead ones The population of red and dead galaxies is building with cosmic time, and it is believed that feedback plays an important role in this process: shutting down star formation by heating and/or expelling the reservoir of cold halo gas To investigate these ideas, we propose to use COS far-UV spectra of background QSOs to measure the properties of the halo gas in a sample of galaxies near the transition mass that have undergone starbursts within the past 100 Myr to 1 Gyr The galactic wind associated with the starburst is predicted to have affected the properties of the gaseous halo To test this, we will compare the properties of the halos of the post-starburst galaxies to those of a control sample of galaxies matched in mass and QSO impact parameter Do the halos of the post-starburst galaxies show a higher incidence rate of Ly-Alpha and metal absorption-lines? Are the kinematics of the halo gas more disturbed in the post-starbursts? Has the wind affected the ionization state and/or the metallicity of the halo? These data will provide fresh new insights into the role of feedback from massive stars on the evolution of galaxies, and may also offer clues about the properties of the QSO metal absorption-line systems at high-redshift

STIS/CCD 11845

CCD Dark Monitor Part 2

Monitor the darks for the STIS CCD

STIS/CCD 11847

CCD Bias Monitor-Part 2

Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns

WFC3/IR 11696

Infrared Survey of Star Formation Across Cosmic Time

We propose to use the unique power of WFC3 slitless spectroscopy to measure the evolution of cosmic star formation from the end of the reionization epoch at z>6 to the close of the galaxy-building era at z~0 3 Pure parallel observations with the grisms have proven to be efficient for identifying line emission from galaxies across a broad range of redshifts The G102 grism on WFC3 was designed to extend this capability to search for Ly-alpha emission from the first galaxies Using up to 250 orbits of pure parallel WFC3 spectroscopy, we will observe about 40 deep (4-5 orbit) fields with the combination of G102 and G141, and about 20 shallow (2-3 orbit) fields with G141 alone

Our primary science goals at the highest redshifts are: (1) Detect Lya in ~100 galaxies with z>5 6 and measure the evolution of the Lya luminosity function, independent of of cosmic variance; 2) Determine the connection between emission line selected and continuum-break selected galaxies at these high redshifts, and 3) Search for the proposed signature of neutral hydrogen absorption at re-ionization At intermediate redshifts we will (4) Detect more than 1000 galaxies in Halpha at 0 5

To identify single-line Lya emitters, we will exploit the wide 0 8--1 9um wavelength coverage of the combined G102+G141 spectra All [OII] and [OIII] interlopers detected in G102 will be reliably separated from true LAEs by the detection of at least one strong line in the G141 spectrum, without the need for any ancillary data We waive all proprietary rights to our data and will make high-level data products available through the ST/ECF

WFC3/IR 12265

Determining the Physical Nature of a Unique Giant Lya Emitter at z=6 595

We propose deep WFC3/IR imaging for a giant Lya emitter (LAE) with a Keck spectroscopic redshift of z=6 595 discovered by extensive narrow-band imaging with Subaru in the SXDS-UKIDSS/UDS field This remarkable object is unique in many respects including its large stellar mass and luminous nebula which extends over 17 kpc; no equivalent source has been found in other surveys The nature of this rare object is unclear Fundamental to progress is determining the origin of star formation in such an early massive object; if the age of the stellar population is short we are likely witnessing a special moment in the formation history of a massive galaxy The heating source for the nebula is also unclear; options include intense star formation, the infall of cold gas onto a dark halo or shock heating from a merger We will take deep broad-band (F125W and F160W) images and an intermediate-band (F098M) image which will be analyzed in conjunction with ultra-deep IRAC 3 6 and 4 5 micron data being taken by the Spitzer/SEDS project These data will enable us to constrain the star formation rate and stellar age Moreover, the UV continuum morphology and Lya-line distribution will be investigated for evidence of a major merger, cold accretion, or hot bubbles associated with outflows We will address the physical origin of the remarkable object observed at an epoch where massive galaxies are thought to begin their assembly

WFC3/IR 12307

A public SNAPSHOT Survey of Gamma-ray Burst Host Galaxies

We propose to conduct a public infrared survey of the host galaxies of Swift selected gamma-ray bursts (GRBs) at z<3 By obtaining deep, diffraction limited imaging in the IR we will complete detections for the host galaxies, and in concert with our extensive ground based afterglow and host programmes will compile a detailed catalog of the properties of high-z galaxies selected by GRBs In particular these observations will enable us to study the colours, luminosities and morphologies of the galaxies This in turn informs studies of the nature of the progenitors and the role of GRBs as probes of star formation across cosmic history Ultimately it provides a product of legacy value which will greatly complement further studies with next generation facilities such as ALMA and JWST

WFC3/IR/S/C 11929

IR Dark Current Monitor

Analyses of ground test data showed that dark current signals are more reliably removed from science data using darks taken with the same exposure sequences as the science data, than with a single dark current image scaled by desired exposure time Therefore, dark current images must be collected using all sample sequences that will be used in science observations These observations will be used to monitor changes in the dark current of the WFC3-IR channel on a day-to-day basis, and to build calibration dark current ramps for each of the sample sequences to be used by Gos in Cycle 17 For each sample sequence/array size combination, a median ramp will be created and delivered to the calibration database system (CDBS)

WFC3/UV 12348

WFC3/UVIS Charge Injection Test

WFC3/UVIS 11905

WFC3 UVIS CCD Daily Monitor

WFC3/UVIS 11908

Cycle 17: UVIS Bowtie Monitor

Ground testing revealed an intermittent hysteresis type effect in the UVIS detector (both CCDs) at the level of ~1%, lasting hours to days Initially found via an unexpected bowtie- shaped feature in flatfield ratios, subsequent lab tests on similar e2v devices have since shown that it is also present as simply an overall offset across the entire CCD, i e , a QE offset without any discernable pattern These lab tests have further revealed that overexposing the detector to count levels several times full well fills the traps and effectively neutralizes the bowtie Each visit in this proposal acquires a set of three 3x3 binned internal flatfields: the first unsaturated image will be used to detect any bowtie, the second, highly exposed image will neutralize the bowtie if it is present, and the final image will allow for verification that the bowtie is gone

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