We extend the stellar-mass gas-phase metallicity relation (MZR) at z = 1.1-3.4 down to the extremely low-mass regime using 183 galaxies with log(M_*/M_⊙) = 6.3-10.2, based on deep JWST/NIRISS slitless spectroscopy from the NGDEEP program. The derived MZR is in excellent agreement with our previous result from 50 galaxies in the GLASS-JWST sample, underscoring the robustness and universality of this relation. Together, these datasets constitute the largest sample of dwarf galaxies yet obtained with NIRISS. The observed MZR slope, β≃0.24±0.03, remains constant across nearly four orders of magnitude in stellar mass. Analytical modeling of the metal-loading factor of outflows (ζ_out) indicates that, at M_*≲10^8M_⊙, ζ_out becomes progressively less dominant than the gas fraction (μ_gas) in regulating the MZR slope. Using this enlarged NIRISS sample, we further test the existence of the fundamental metallicity relation (FMR). We find no robust evidence for an additional SFR dependence beyond the MZR, nor any reduction in metallicity scatter when SFR is included. Examination of systematic uncertainties in , M_* and SFR suggests that the MZR slope (β∼0.22) is robust, and that different assumptions about the strong-line calibrations or star-formation history (SFH) of the galaxies change the slope by less than 1-σ. At the current depth of the NIRISS data, evidence for an FMR among high-redshift dwarf galaxies remains inconclusive, highlighting the need for larger samples, and deeper observations.

We present the Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE) spectroscopic redshift catalog in the COSMOS field. PASSAGE is a JWST Cycle 1 Near Infrared Imager and Slitless Spectrograph (or NIRISS) wide-field slitless spectroscopy pure-parallel survey, obtaining near-infrared spectra of thousands of extragalactic sources. Fifteen out of 63 PASSAGE fields fall within the Hubble Space Telescope COSMOS footprint, of which 11 overlap with COSMOS-Web, a JWST treasury survey providing additional space-based photometry. We present our custom line-finding algorithm and visual inspection effort used to identify emission lines and derive the spectroscopic redshifts for line-emitting sources in PASSAGE. The line-finding algorithm identifies between similar to 200 and 950 line-emitting candidates per field, of which typically 47% were identified as true emission lines post visual inspection. We identify 2183 emission-line sources at 0.08 less than or similar to z less than or similar to 4.7, 1896 of which have available COSMOS photometric redshifts. We find excellent redshift agreement between the COSMOS photometric redshifts and the PASSAGE spectroscopic redshifts for strong (signal-to-noise ratio > 5), multi-line-emitting sources. This agreement weakens for PASSAGE single-line emitters with ambiguous identities. These single-line emitters are likely misidentified around 18% of the time based on comparisons to photometric redshifts. We derive stellar masses using PASSAGE photometry and spectroscopic redshifts, in broad agreement with existing COSMOS-Web stellar masses, but with some discrepancy driven by redshift disagreements. We publicly release this spectroscopic redshift catalog, which will enable community-led science in prime extragalactic fields and serve as a crucial dataset for validating Euclid and Roman spectroscopy.

Abstract We analyze spectroscopy from one NIRISS pointing in the JWST-Parallel Application of Slitless Spectroscopic to Analyze Galaxy Evolution program for seven candidate z ≳ 7.5 photometrically selected COSMOS-Web sources. We spectroscopically confirm one out of seven sources as a Lyman break galaxy at z = 7.96 2 − 0.006 + 0.003 , with m F150W = 25.9 (AB). The remaining sources are too faint in the continuum (i.e., m F150W ≳ 26 AB) to provide a redshift measurement from the Lyman break, and do not show emission lines in their spectra. Although this study contains only one spectroscopically confirmed source, the confirmation of a luminous z ∼ 8 galaxy within this ∼4.8 arcmin 2 field implies a surface density of ∼ 0.2 1 − 0.17 + 0.59 arcmin −2 , ≈10× higher than inferred from wide-area photometric surveys, suggesting a potential overdensity at z ∼ 8 in the COSMOS field.

The virial coefficient (f), which is meant to encapsulate broad-line region (BLR) geometry and kinematics, remains one of the largest sources of systematic uncertainty in black hole mass estimates for Active Galactic Nuclei (AGNs). While the use of a sample average ⟨ f ⟩ enables black hole mass estimates across large samples and cosmological distances, individual AGNs may deviate from this average due to differences in BLR structure and viewing angle. In previous work, we reported marginal evidence for a correlation between f and the shape of the broad Hβ emission line, log_10(FWHM/σ). In this work, we update our sample to include ten new sources with CARAMEL BLR dynamical modeling, increasing both the black hole mass range and statistical power of our analysis. We find marginal evidence for a correlation between f and log_10(FWHM/σ), with a slope and intrinsic scatter consistent with previous results. The confirmation of this trend across a larger sample further supports the idea that line profile shape may reflect BLR properties in a way that directly impacts f. If confirmed with future BLR dynamical modeling of sources within a wider range of log_10(FWHM/σ), this relationship could enable empirical estimates of the virial coefficient and improve single-epoch black hole mass estimates across cosmic time.

Ram pressure stripping (RPS) plays a crucial role in shaping galaxy evolution in dense environments, yet its impact on the molecular and dusty phases of the interstellar medium remains poorly understood. We present JWST/NIRCam 3.3μm polycyclic aromatic hydrocarbon (PAH) emission maps for the nine most striking RPS galaxies in the Abell 2744 cluster at redshift z_cl=0.306, tracing the effects of environmental processes on small dust grains. Exploiting multi-band JWST/NIRCam and HST photometry, we performed a spatially resolved ultraviolet (UV) to mid-infrared (MIR) spectral energy distribution (SED) fitting to characterise stellar populations in both galactic disks and clumps detected in the stripped tails. We detected PAH_3.3 emission in eight of the nine galaxies at 5σ, with morphologies revealing disk truncation and elongation along the RPS direction. In three galaxies, PAH_3.3 emission is also found in star-forming clumps embedded in the stripped tails up to a distance of 40kpc. Star formation rates inferred from PAH_3.3 emission are in agreement with those derived from SED fitting averaged over the past 100Myr within an intrinsic scatter of 0.4dex, but the relation appears to be age-dependent. The spatial correlation between the PAH strength, stellar age, and star formation rate (SFR) is consistent across disks and tails and demonstrates that PAH-carrying molecules can survive and become stripped by ram pressure. Finally, age gradients revealed by the SED fitting provide observational evidence of the fireball model in star-forming, stripped clumps of galaxies at z ∼ 0.3. This work represents the first detailed study of PAH emission in cluster galaxies, offering new insights into the fate of dust and star formation in extreme environments.

Using JWST/NIRISS slitless spectroscopy, we present spatially resolved Balmer decrement measurements for 79 galaxies at 1.1 < z < 2.3, which are gravitationally lensed by the foreground cluster A2744. By stacking H alpha and H beta emission maps in bins of stellar mass and redshift, we derive radial profiles of nebular dust attenuation and dust-corrected star formation rate (SFR). We find tentative evidence that the radial gradients of dust attenuation toward H alpha (A(H alpha)) vary with both redshift and stellar mass. At lower redshifts (z = 1.10-1.53), low-mass galaxies ( 7.0 < log(M-*/M-circle dot) <= 8.5 ) exhibit steeper A(H alpha) gradients than higher-mass galaxies ( 9.5 < log (M-*/M-circle dot) <= 11.0 ), while the latter maintain detectable dust attenuation out to larger galactocentric radii. Galaxies at higher redshifts (z = 1.76-2.29) show lower attenuation levels. At fixed galactocentric radius, galaxies in the low-redshift bin generally exhibit higher dust attenuation than those at high redshifts, consistent with an increase in dust content toward later cosmic times. Dust-corrected SFR profiles in massive systems at lower redshifts are more spatially extended than those at higher redshifts, consistent with inside-out disk growth at z less than or similar to 1.5. These results suggest possible differences in attenuation properties across stellar mass and redshift bins, and demonstrate the power of gravitational lensing to probe internal structures in faint galaxies at subkiloparsec resolution.

Spatially resolved gas-phase metallicity maps are a crucial element in building our understanding of the chemical evolution of galaxies. We present spatially resolved metallicity maps obtained from NIRISS/WFSS observations in the first work delivering such an analysis of the slitless spectroscopy of multiple galaxies. We investigated the sources of ionization, metallicity, and their relation to star formation in a spatially resolved sense for a sample of eight galaxies: four from JWST-PASSAGE and four from GLASS-JWST ERS. All but one of these galaxies reside in the redshift range 1.9 ≤ z ≤ 2, the outlier being at z = 3.1. Our sample covers a range of 8.0 < log (M ⋆ / M ⊙ ) < 9.5 in terms of stellar mass, 0.2 < log (SFR M ⊙ yr −1 ) < 1.1 in the star formation rate (SFR), and 7.8 < 12 + log(O / H) < 9.0 in the global gas metallicity. To resolve the question of the star formation-AGN separation in the absence of resolved H α +[NII] lines, we present a new SF-demarcation line in the OHNO parameter space, based on MAPPINGS v5.1 publicly available H II region and AGN model grids, with the caveat that these grids partially overlap the OHNO parameter space. We present the mass-metallicity gradient relation for our sample, which show no clear trend with stellar mass. This might be because the high- z galaxies have not yet started their accretion-dominated evolutionary phase. By interpreting the correlation between spatially resolved metallicity and SFR maps as a proxy for effective timescales of metal-transport in galaxies, we find a possible trend that sees this timescale increasing with stellar mass. This is consistent with the picture of more effective feedback in lower mass galaxies and where massive galaxies generally tend to have longer characteristic timescales.

Environment plays a crucial role in shaping galaxy formation, yet the impact of overdensities on the internal chemical structure of galaxies at cosmic noon is still under debate. Here, we present spatially resolved gas-phase metallicity gradients for 42 star-forming galaxies in three massive protoclusters at z ∼ 2.3, derived fromHubble Space Telescope (HST) slitless grism spectroscopy from the MAMMOTH-Grism survey. We find that the majority (29 of 42, ∼69

We present H alpha luminosity function (LF) measurements at redshifts z similar to 1.3 and z similar to 2.0 using JWST NIRISS grism data from the GLASS-JWST survey. Based on emission lines spectroscopically identified in the F115W, F150W, and F200W filters, we select 99 H alpha emitters. Through a detailed effective volume and completeness analysis for each source, we construct the H alpha LF in two redshift bins. Thanks to the sensitivity of NIRISS WFSS and gravitational lensing magnification, our sample reaches intrinsic H alpha luminosities similar to 10 times deeper than previous grism surveys, down to LH alpha similar to 1040.5 erg s-1 at z similar to 1.3 and LH alpha similar to 1040.9 erg s-1 at z similar to 2.0 with a completeness larger than 0.8, corresponding to star formation rates of 0.4 and 1.0 M circle dot yr-1, respectively. We robustly constrain the faint-end slope of the H alpha LF to be -1.50-0.08+0.14 at z similar to 1.3 and -1.60-0.09+0.17 at z similar to 2.0 after considering the cosmic variance of similar to 20%, consistent with previous estimations. The emission-line samples presented here will enable further detailed studies of galaxy properties including metallicities. We find a negligible contribution from bright active galactic nuclei in our sample. We estimate integrated cosmic star formation rate densities of 0.097-0.016+0.015M circle dot yr-1Mpc-3 at z similar to 1.3 and 0.129-0.030+0.025M circle dot yr-1Mpc-3 at z similar to 2.0. The methodology presented here can be readily applicable to other JWST slitless spectroscopic datasets and future wide-field slitless surveys, including those from Euclid, Roman, and the Chinese Space Station Telescope.

We present one of the first measurements of the mass-metallicity relation (MZR) in multiple massive protoclusters at cosmic noon, using Hubble Space Telescope (HST) G141 slitless spectroscopy from the MAMMOTH-Grism survey. We identify 63 protocluster member galaxies across three overdense structures at z = 2-3 with robust detections of [O iii], H beta, and [O ii] emission. The sample spans gas-phase metallicities of 12+log(O/H)=8.2-8.6 , dust-corrected H beta-based star formation rates (SFRs) of 10-250 M-circle dot yr(-1), and stellar masses of M* similar to 10(9.4)-10(10.5) M-circle dot, derived via spectral energy distribution fitting using deep HST and ground-based photometry. We stack spectra in five M(*)bins to obtain average metallicities and SFRs. Relative to field galaxies at similar redshifts, protocluster members show elevated SFRs at M-* < 10(10.25) M-circle dot and a systematically shallower MZR: 12+log(O/H) =(6.96 +/- 0.13) + (0.143 +/- 0.017) xlog(M-*/M-circle dot) . We detect a mass-dependent environmental offset: massive protocluster galaxies are metal-poor compared to field counterparts of similar mass, whereas lower-mass systems exhibit comparable or mildly enhanced metallicities. This trend is consistent with a scenario where cold-mode accretion dilutes the interstellar medium (ISM) across the full mass range, while efficient recycling of feedback-driven outflows preferentially enriches the ISM in low-mass galaxies. Finally, we assess the dependence of metallicity offsets on local overdensity and find no significant trend, likely reflecting the survey's bias toward protocluster cores.

Reverberation mapping (RM) determines the mass of black holes (BHs) in active galactic nuclei (AGNs) by resolving the BH gravitational sphere of influence in the time domain. Recent RM campaigns have yielded direct BH masses through dynamical modeling for a sample of 32 objects, spanning a wide range of AGN luminosities and BH masses. In addition, accurate BH masses have been determined by spatially resolving the broad-line region with GRAVITY for a handful of AGNs. Here, we present a detailed analysis of Hubble Space Telescope images using surface-brightness profile fitting with state-of-the-art programs. We derive AGN luminosity and host-galaxy properties, such as radii and luminosities for the spheroid, disk, and bar (if present). The spheroid effective radii are used to measure stellar velocity dispersion from integral-field spectroscopy. Since the BH masses of our sample do not depend on any assumption of the virial factor needed in single-epoch spectroscopic mass estimates, we can show that the resulting scaling relations between the mass of the supermassive BHs and their host galaxies match those of quiescent galaxies, naturally extending to lower masses in these (predominantly) spiral galaxies. We find that the inner AGN orientation, as traced by the broad-line region inclination angle, is uncorrelated with the host-galaxy disk. Our sample has the most direct and accurate M _BH measurements of any AGN sample and provides a fundamental local benchmark for studies of the evolution of massive BHs and their host galaxies across cosmic time.

To reproduce observed galaxy properties, cosmological simulations require that massive galaxies experience feedback from active galactic nuclei, which regulates star formation within those galaxies. However, the energetics and timescales of these feedback processes are poorly constrained. We combined optical, infrared, submillimeter, and radio observations of the active galaxy VV 340a, which is hosting a low-power jet launched from a supermassive black hole at its center. We found that the jet undergoes precession, with a period of (8.2 ± 5.5) × 105 years, and drives an outflow of gas at a rate of 19.4 ± 7.9 solar masses per year. The jet shocks the gas, producing highly ionized plasma that extends several kiloparsecs from the nucleus. The outflow ejects sufficient gas from the galaxy to influence its star-formation rate.

We present new and archival Atacama Large Millimeter/submillimeter Array observations of two strongly lensed dusty star-forming galaxies (DSFGs) selected from the South Pole Telescope survey, SPT0418-47 ( z = 4.225) and SPT2147-50 ( z = 3.760). We study the [C ii ], CO(7–6), [C i ](2–1), and, in SPT0418-47, p –H _2 O emission, which, along with the underlying continuum (rest-frame 160 and 380 μ m), are routinely used as tracers of gas mass and/or star-formation rate (SFR). We perform a pixel-by-pixel analysis of both sources in the image plane to study the resolved Kennicutt–Schmidt relation, finding generally good agreement between the slopes of the SFR versus gas mass surface density using the different tracers. Using lens modeling methods, we find that the dust emission is more compact than the line emission in both sources, with CO(7–6) and [C i ](2–1) similar in extent and [C ii ] the most extended, reminiscent of recent findings of extended [C ii ] spatial distributions in galaxies at similar cosmic epochs. We develop the [C i ](2–1)/ CO(7–6) flux-density ratio as an observable proxy for gas depletion timescale ( τ _dep ), which can be applied to large samples of DSFGs, in lieu of more detailed inferences of this timescale, which require analysis of observations at multiple wavelengths. Furthermore, the extended [C ii ] emission in both sources, compared to the total continuum and line emission, suggests that [C ii ], used in recent years as a molecular gas mass and SFR tracer in high- z galaxies, may not always be a suitable tracer of these physical quantities.

We investigate the connection between ionized gas kinematics and gas-phase metallicity gradients in 21 star-forming galaxies at 0.5 < z < 1.7 from the MSA-3D survey, using spatially resolved JWST/NIRSpec slit-stepping observations. Galaxy kinematics are characterized by the ratio of rotational velocity to intrinsic velocity dispersion, v/sigma, measured at 1.5 R-e, where R-e is the effective radius. We find that dynamically hotter disks exhibit systematically flatter metallicity gradients, with a moderate anticorrelation between del O/H and v/sigma ( rho=-0.30(-0.15)(+0.16) ). A linear fit yields a slope of similar to 0.005 dex per dex in v/sigma, weaker than the dependence on stellar mass. Similarly, the N2 gradients show a consistent trend, with rho(v/sigma,del N2)=-0.23(-0.08)(+0.07) , indicating that the correlation is robust to the choice of metallicity indicator. A significantly stronger anticorrelation is observed with Re/sigma, interpreted as a proxy for the radial mixing timescale (Spearman rank correlation coefficient rho=-0.43(-0.13)(+0.14) ), suggesting that cumulative radial mixing more directly regulates chemical stratification. The metallicity gradients in our sample are uniformly shallow, indicating that efficient turbulent mixing in kinematically settled disks regulates the chemical structure of typical star-forming galaxies at z similar to 1.

The virial coefficient (f), which is meant to encapsulate broad-line region (BLR) geometry and kinematics, remains one of the largest sources of systematic uncertainty in black hole mass estimates for active galactic nuclei (AGNs). While the use of a sample average < f > enables black hole mass estimates across large samples and cosmological distances, individual AGNs may deviate from this average due to differences in BLR structure and viewing angle. In previous work, we reported marginal evidence for a correlation between f and the shape of the broad H beta emission line, log10(FWHM/sigma) . In this work, we update our sample to include 10 new sources with CARAMEL BLR dynamical modeling, increasing both the black hole mass range and statistical power of our analysis. We find marginal evidence for a correlation between f and log10(FWHM/sigma) , with a slope and intrinsic scatter consistent with previous results. The confirmation of this trend across a larger sample further supports the idea that line profile shape may reflect BLR properties in a way that directly impacts f. If confirmed with future BLR dynamical modeling of sources within a wider range of log10(FWHM/sigma) , this relationship could enable empirical estimates of the virial coefficient and improve single-epoch black hole mass estimates across cosmic time.

In the nearby Universe, the environment plays a crucial role in suppressing star formation in dense regions. In particular, ram-pressure stripping (RPS) is a major mechanism for removing gas from galaxies in clusters, occurring when galaxies travel through a dense hot atmosphere and leave trailing gaseous wakes. By depleting the cold gas reservoir, RPS can drive outside-in quenching and is therefore thought to be an important route for transforming cluster galaxies. At earlier times, however, protoclusters are dynamically young and their hot atmospheres are expected to be immature, so environmental effects are commonly assumed to be dominated by gravitational interactions rather than hydrodynamic stripping. Recent observations have begun to show that RPS can already operate before mature cluster assembly, including extended gas tails in a forming cluster at z=2.51 and in a galaxy group at z=3.06. These studies demonstrate that hydrodynamic stripping is possible at earlier times, but whether RPS can become sufficient enough to quench massive galaxies at z>2 remains unclear. Here we report ALMA and JWST observations of SPT2349-56-C26, a massive galaxy experiencing an extreme RPS event in the SPT2349-56 protocluster at z=4.30. C26 appears to exhibit a particularly severe active-stripping phase: the displaced gas contains more than half of the observed cold-gas reservoir, with the gas-emission peak showing a large 6-kpc offset from the stellar body. These observations show that RPS can remove most of the cold gas from massive galaxies in dense protocluster cores as early as z=4.3, providing a direct hydrodynamic pathway for environmental quenching at z>4.

We analyzed a large sample of Sloan Digital Sky Survey spectra of Seyfert galaxies, subdividing type 1 Seyferts (Sy1s) based on their narrow to broad H α components. Comparing their narrow lines (NLs) to type 2 Seyferts (Sy2s) in line-ratio diagrams, most of the NLs of strong Sy1.0/Sy1.2s (with dominant broad lines) are the same as those of “pure” Sy2s. In contrast, only ∼25%–30% of the Sy1.8 and Sy1.9 nuclei (with weak broad lines) are located in the pure Sy2 region, with the rest falling in the composite/star-forming region. We explain these Seyfert+star formation spectra with a simple model. It shows that 85% of NLs in Sy1.9s are from H II regions, while 88% of the NLs in Sy1.0s arise from the same narrow-line region as in pure Sy2s. About ∼6% of the strong and weak Sy1s have NLs dominated by low-ionization nuclear emission-line region (LINER) emission, while ∼15% of intermediate Seyferts (Sy1.5/Sy1.6) do. To confirm this Seyfert 1 active galactic nucleus (AGN)+star formation combination, we used stellar absorption lines to compare their stellar populations. Their H δ strengths show that LINERs, pure Sy2s, and also the broad-line-dominated Sy1s have old stellar populations. The weak Sy1s show stronger H δ absorption, indicating larger proportions of young stars. About one-third of the u -band light in Sy1.0/1.2s is blended Balmer lines and continuum from the broad-line region (BLR). The NL gas reddening increases as the BLR strength decreases, from Sy1.0 (0.13 mag) to Sy1.9 (0.40 mag), to Sy2s and LINERs, both with 0.50 mag. Our data do not support the simplest version of Seyfert 1 and 2 unification, where both AGN classes have identical NLs.

We analyze spectroscopy from one NIRISS pointing in the JWST-PASSAGE program for seven candidate z ≳ 7.5 photometrically-selected COSMOS-Web sources. We spectroscopically confirm one out of seven sources as a Lyman break galaxy (LBG) at z=7.962^+0.003_-0.006, with m_F150W = 25.9 (AB). The remaining sources are too faint in the continuum (i.e., m_F150W≳ 26 AB) to provide a redshift measurement from the Lyman break, and do not show emission lines in their spectra. Although this study contains only one spectroscopically confirmed source, the confirmation of a luminous z ∼ 8 galaxy within this ∼4.8 arcmin^2 field implies a surface density of ∼ 0.21^+0.59_-0.17 arcmin^-2, ≈ 10× higher than inferred from wide-area photometric surveys, suggesting a potential overdensity at z∼8 in the COSMOS field.

The origin of the tight scaling relation between the mass of supermassive black holes (SMBHs; M BH) and their host-galaxy properties remains unclear. Active galactic nuclei (AGNs) probe phases of ongoing SMBH growth and offer the only opportunity to measure M BH beyond the local Universe. However, determining an AGN's host galaxy's stellar velocity dispersion, sigma star, and its galaxy dynamical mass, M dyn, is complicated by AGN contamination, aperture effects, and different host-galaxy morphologies. We select a sample of AGNs for which M BH has been independently determined to high accuracy by state-of-the-art techniques: dynamical modeling of the reverberation signal and spatially resolving the broad-line region with the Very Large Telescope Interferometer/GRAVITY. Using integral-field spectroscopic observations, we spatially map the host-galaxy stellar kinematics across the galaxy and bulge effective radii. We find that the dynamically hot component of galaxy disks correlates with M BH; however, the correlations are tightest for aperture-integrated sigma star measured across the bulge. Accounting for the different M BH distributions, we demonstrate-for the first time-that AGNs follow the same M BH-sigma star and M BH-M bulge,dyn relations as quiescent galaxies. We confirm that the classical approach of determining the virial factor as a sample average, yielding logf=0.65 +/- 0.18 , is consistent with the average f from individual measurements. The similarity between the underlying scaling relations of AGNs and quiescent galaxies implies that the current AGN phase is too short to have altered black hole masses on a population level. These results strengthen the local calibration of f for measuring single-epoch M BH in the distant Universe.

We introduce a prescription for estimating the flux of the 7.7 micron and 11.3 micron polycyclic aromatic hydrocarbon (PAH) features from broadband JWST/MIRI images. Probing PAH flux with MIRI imaging data has advantages in field of view, spatial resolution, and sensitivity compared with MIRI spectral maps, but comparisons with spectra are needed to calibrate these flux estimations over a wide variety of environments. For 267 MIRI/MRS spectra from independent regions in the four luminous infrared galaxies (LIRGs) in the Great Observatories All-sky LIRG Survey (GOALS) early release science program, we derive synthetic filter photometry and directly compare estimated PAH fluxes to those measured from detailed spectral fits. We find that for probing PAH 7.7 micron, the best combination of filters is F560W, F770W, and either F1500W or F2100W, and the best for PAH 11.3 micron is F560W, F1000W, F1130W, and F1500W. The prescription with these combinations yields predicted flux densities that typically agree with values from spectral decomposition within 7 PAH 7.7 and 11.3 micron, respectively.