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Author

Duilia F. de Mello

Bio: Duilia F. de Mello is an academic researcher from The Catholic University of America. The author has contributed to research in topics: Galaxy & Star formation. The author has an hindex of 47, co-authored 147 publications receiving 18220 citations. Previous affiliations of Duilia F. de Mello include Chalmers University of Technology & California Institute of Technology.


Papers
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Journal ArticleDOI
TL;DR: Starburst99 as mentioned in this paper is a comprehensive set of model predictions for spectrophotometric and related properties of galaxies with active star formation, which is an improved and extended version of the data set previously published by Leitherer & Heckman.
Abstract: Starburst99 is a comprehensive set of model predictions for spectrophotometric and related properties of galaxies with active star formation. The models are an improved and extended version of the data set previously published by Leitherer & Heckman. We have upgraded our code by implementing the latest set of stellar evolution models of the Geneva group and the model atmosphere grid compiled by Lejeune et al. Several predictions which were not included in the previous publication are shown here for the first time. The models are presented in a homogeneous way for five metallicities between Z = 0.040 and 0.001 and three choices of the initial mass function. The age coverage is 106—109 yr. We also show the spectral energy distributions which are used to compute colors and other quantities. The full data set is available for retrieval at a Web site, which allows users to run specific models with nonstandard parameters as well. We also make the source code available to the community.

4,212 citations

Journal ArticleDOI
Norman A. Grogin1, Dale D. Kocevski2, Sandra M. Faber2, Henry C. Ferguson1, Anton M. Koekemoer1, Adam G. Riess3, Viviana Acquaviva4, David M. Alexander5, Omar Almaini6, Matthew L. N. Ashby7, Marco Barden8, Eric F. Bell9, Frédéric Bournaud10, Thomas M. Brown1, Karina Caputi11, Stefano Casertano1, Paolo Cassata12, Marco Castellano, Peter Challis7, Ranga-Ram Chary13, Edmond Cheung2, Michele Cirasuolo14, Christopher J. Conselice6, Asantha Cooray15, Darren J. Croton16, Emanuele Daddi10, Tomas Dahlen1, Romeel Davé17, Duilia F. de Mello18, Duilia F. de Mello19, Avishai Dekel20, Mark Dickinson, Timothy Dolch3, Jennifer L. Donley1, James Dunlop11, Aaron A. Dutton21, David Elbaz10, Giovanni G. Fazio7, Alexei V. Filippenko22, Steven L. Finkelstein23, Adriano Fontana, Jonathan P. Gardner18, Peter M. Garnavich24, Eric Gawiser4, Mauro Giavalisco12, Andrea Grazian, Yicheng Guo12, Nimish P. Hathi25, Boris Häussler6, Philip F. Hopkins22, Jiasheng Huang26, Kuang-Han Huang3, Kuang-Han Huang1, Saurabh Jha4, Jeyhan S. Kartaltepe, Robert P. Kirshner7, David C. Koo2, Kamson Lai2, Kyoung-Soo Lee27, Weidong Li22, Jennifer M. Lotz1, Ray A. Lucas1, Piero Madau2, Patrick J. McCarthy25, Elizabeth J. McGrath2, Daniel H. McIntosh28, Ross J. McLure11, Bahram Mobasher29, Leonidas A. Moustakas13, Mark Mozena2, Kirpal Nandra30, Jeffrey A. Newman31, Sami Niemi1, Kai G. Noeske1, Casey Papovich23, Laura Pentericci, Alexandra Pope12, Joel R. Primack2, Abhijith Rajan1, Swara Ravindranath32, Naveen A. Reddy29, Alvio Renzini, Hans-Walter Rix30, Aday R. Robaina33, Steven A. Rodney3, David J. Rosario30, Piero Rosati34, S. Salimbeni12, Claudia Scarlata35, Brian Siana29, Luc Simard36, Joseph Smidt15, Rachel S. Somerville4, Hyron Spinrad22, Amber Straughn18, Louis-Gregory Strolger37, Olivia Telford31, Harry I. Teplitz13, Jonathan R. Trump2, Arjen van der Wel30, Carolin Villforth1, Risa H. Wechsler38, Benjamin J. Weiner17, Tommy Wiklind39, Vivienne Wild11, Grant W. Wilson12, Stijn Wuyts30, Hao Jing Yan40, Min S. Yun12 
TL;DR: The Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) as discussed by the authors was designed to document the first third of galactic evolution, from z approx. 8 - 1.5 to test their accuracy as standard candles for cosmology.
Abstract: The Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) is designed to document the first third of galactic evolution, from z approx. 8 - 1.5. It will image > 250,000 distant galaxies using three separate cameras on the Hubble Space Tele8cope, from the mid-UV to near-IR, and will find and measure Type Ia supernovae beyond z > 1.5 to test their accuracy as standard candles for cosmology. Five premier multi-wavelength sky regions are selected, each with extensive ancillary data. The use of five widely separated fields mitigates cosmic variance and yields statistically robust and complete samples of galaxies down to a stellar mass of 10(exp 9) solar mass to z approx. 2, reaching the knee of the UV luminosity function of galaxies to z approx. 8. The survey covers approximately 800 square arc minutes and is divided into two parts. The CANDELS/Deep survey (5(sigma) point-source limit H =27.7mag) covers approx. 125 square arcminutes within GOODS-N and GOODS-S. The CANDELS/Wide survey includes GOODS and three additional fields (EGS, COSMOS, and UDS) and covers the full area to a 50(sigma) point-source limit of H ? or approx. = 27.0 mag. Together with the Hubble Ultradeep Fields, the strategy creates a three-tiered "wedding cake" approach that has proven efficient for extragalactic surveys. Data from the survey are non-proprietary and are useful for a wide variety of science investigations. In this paper, we describe the basic motivations for the survey, the CANDELS team science goals and the resulting observational requirements, the field selection and geometry, and the observing design.

2,088 citations

Journal ArticleDOI
Anton M. Koekemoer1, Sandra M. Faber2, Henry C. Ferguson1, Norman A. Grogin1, Dale D. Kocevski2, David C. Koo2, Kamson Lai2, Jennifer M. Lotz1, Ray A. Lucas1, Elizabeth J. McGrath2, Sara Ogaz1, Abhijith Rajan1, Adam G. Riess3, S. Rodney3, L. G. Strolger4, Stefano Casertano1, Marco Castellano, Tomas Dahlen1, Mark Dickinson, Timothy Dolch3, Adriano Fontana, Mauro Giavalisco5, Andrea Grazian, Yicheng Guo5, Nimish P. Hathi6, Kuang-Han Huang3, Kuang-Han Huang1, Arjen van der Wel7, Hao Jing Yan8, Viviana Acquaviva9, David M. Alexander10, Omar Almaini11, Matthew L. N. Ashby12, Marco Barden13, Eric F. Bell14, Frédéric Bournaud15, Thomas M. Brown1, Karina Caputi16, Paolo Cassata5, Peter Challis17, Ranga-Ram Chary18, Edmond Cheung2, Michele Cirasuolo16, Christopher J. Conselice11, Asantha Cooray19, Darren J. Croton20, Emanuele Daddi15, Romeel Davé21, Duilia F. de Mello22, Loic de Ravel16, Avishai Dekel23, Jennifer L. Donley1, James Dunlop16, Aaron A. Dutton24, David Elbaz25, Giovanni Fazio12, Alexei V. Filippenko26, Steven L. Finkelstein27, Chris Frazer19, Jonathan P. Gardner22, Peter M. Garnavich28, Eric Gawiser9, Ruth Gruetzbauch11, Will G. Hartley11, B. Haussler11, Jessica Herrington14, Philip F. Hopkins26, J.-S. Huang29, Saurabh Jha9, Andrew Johnson2, Jeyhan S. Kartaltepe3, Ali Ahmad Khostovan19, Robert P. Kirshner12, Caterina Lani11, Kyoung-Soo Lee30, Weidong Li26, Piero Madau2, Patrick J. McCarthy6, Daniel H. McIntosh31, Ross J. McLure, Conor McPartland2, Bahram Mobasher32, Heidi Moreira9, Alice Mortlock11, Leonidas A. Moustakas18, Mark Mozena2, Kirpal Nandra33, Jeffrey A. Newman34, Jennifer L. Nielsen31, Sami Niemi1, Kai G. Noeske1, Casey Papovich27, Laura Pentericci, Alexandra Pope, Joel R. Primack2, Swara Ravindranath35, Naveen A. Reddy, Alvio Renzini, Hans Walter Rix7, Aday R. Robaina, David J. Rosario2, Piero Rosati7, S. Salimbeni5, Claudia Scarlata18, Brian Siana18, Luc Simard36, Joseph Smidt19, D. Snyder2, Rachel S. Somerville1, Hyron Spinrad26, Amber N. Straughn22, Olivia Telford34, Harry I. Teplitz18, Jonathan R. Trump2, Carlos J. Vargas9, Carolin Villforth1, C. Wagner31, P. Wandro2, Risa H. Wechsler37, Benjamin J. Weiner21, Tommy Wiklind1, Vivienne Wild, Grant W. Wilson5, Stijn Wuyts12, Min S. Yun5 
TL;DR: In this paper, the authors describe the Hubble Space Telescope imaging data products and data reduction procedures for the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS).
Abstract: This paper describes the Hubble Space Telescope imaging data products and data reduction procedures for the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). This survey is designed to document the evolution of galaxies and black holes at z 1.5-8, and to study Type Ia supernovae at z > 1.5. Five premier multi-wavelength sky regions are selected, each with extensive multi-wavelength observations. The primary CANDELS data consist of imaging obtained in the Wide Field Camera 3 infrared channel (WFC3/IR) and the WFC3 ultraviolet/optical channel, along with the Advanced Camera for Surveys (ACS). The CANDELS/Deep survey covers ~125 arcmin2 within GOODS-N and GOODS-S, while the remainder consists of the CANDELS/Wide survey, achieving a total of ~800 arcmin2 across GOODS and three additional fields (Extended Groth Strip, COSMOS, and Ultra-Deep Survey). We summarize the observational aspects of the survey as motivated by the scientific goals and present a detailed description of the data reduction procedures and products from the survey. Our data reduction methods utilize the most up-to-date calibration files and image combination procedures. We have paid special attention to correcting a range of instrumental effects, including charge transfer efficiency degradation for ACS, removal of electronic bias-striping present in ACS data after Servicing Mission 4, and persistence effects and other artifacts in WFC3/IR. For each field, we release mosaics for individual epochs and eventual mosaics containing data from all epochs combined, to facilitate photometric variability studies and the deepest possible photometry. A more detailed overview of the science goals and observational design of the survey are presented in a companion paper.

2,011 citations

Journal ArticleDOI
Anton M. Koekemoer, Sandra M. Faber, Henry C. Ferguson, Norman A. Grogin, Dale D. Kocevski, David C. Koo, Kamson Lai, Jennifer M. Lotz, Ray A. Lucas, Elizabeth J. McGrath, Sara Ogaz, Abhijith Rajan, Adam G. Riess, S. Rodney, Louis Gregory Strolger, Stefano Casertano, Marco Castellano, Tomas Dahlen, Mark Dickinson, Timothy Dolch, Adriano Fontana, Mauro Giavalisco, Andrea Grazian, Yicheng Guo, Nimish P. Hathi, Kuang-Han Huang, Arjen van der Wel, Haojing Yan, Viviana Acquaviva, David M. Alexander Omar Almaini, Matthew L. N. Ashby, Marco Barden, Eric F. Bell, Frédéric Bournaud, Thomas M. Brown, Karina Caputi, Paolo Cassata, Peter Challis, Ranga-Ram Chary, Edmond Cheung, Michele Cirasuolo, Christopher J. Conselice, Asantha Cooray, Darren J. Croton, Emanuele Daddi, Romeel Davé, Duilia F. de Mello, Loic de Ravel, Avishai Dekel, Jennifer L. Donley, James Dunlop, Aaron A. Dutton, David Elbaz, Giovanni G. Fazio, Alex V. Filippenko, Steven L. Finkelstein, Chris Frazer, Jonathan P. Gardner, Peter M. Garnavich, Eric Gawiser, Ruth Gruetzbauch, Will G. Hartley, Boris Häussler, Jessica Herrington, Philip F. Hopkins, Jiasheng Huang, Saurabh Jha, Andrew Johnson, Jeyhan S. Kartaltepe, Ali Ahmad Khostovan, Robert P. Kirshner, Caterina Lani, Kyoung-Soo Lee, Weidong Li, Piero Madau, Patrick J. McCarthy, Daniel H. McIntosh, Ross J. McLure, Conor McPartland, Bahram Mobasher, Heidi Moreira, Alice Mortlock, Leonidas A. Moustakas, Mark Mozena, Kirpal Nandra, Jeffrey A. Newman, Jennifer L. Nielsen, Sami Niemi, Kai G. Noeske, Casey Papovich, Laura Pentericci, Alexandra Pope, Joel R. Primack, Swara Ravindranath, Naveen A. Reddy, Alvio Renzini, Hans-Walter Rix, Aday R. Robaina, David J. Rosario, Piero Rosati, S. Salimbeni, Claudia Scarlata, Brian Siana, Luc Simard, Joseph Smidt, D. Snyder, Rachel S. Somerville, Hyron Spinrad, Amber Straughn, Olivia Telford, Harry I. Teplitz, Jonathan R. Trump, Carlos J. Vargas, Carolin Villforth, C. Wagner, P. Wandro, Risa H. Wechsler, Benjamin J. Weiner, Tommy Wiklind, Vivienne Wild, Grant W. Wilson, Stijn Wuyts, Min S. Yun 
TL;DR: The Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) as mentioned in this paper was designed to document the evolution of galaxies and black holes at $z\sim 1.5-8$, and to study Type Ia SNe beyond $z>1.5.
Abstract: This paper describes the Hubble Space Telescope imaging data products and data reduction procedures for the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS). This survey is designed to document the evolution of galaxies and black holes at $z\sim1.5-8$, and to study Type Ia SNe beyond $z>1.5$. Five premier multi-wavelength sky regions are selected, each with extensive multiwavelength observations. The primary CANDELS data consist of imaging obtained in the Wide Field Camera 3 / infrared channel (WFC3/IR) and UVIS channel, along with the Advanced Camera for Surveys (ACS). The CANDELS/Deep survey covers \sim125 square arcminutes within GOODS-N and GOODS-S, while the remainder consists of the CANDELS/Wide survey, achieving a total of \sim800 square arcminutes across GOODS and three additional fields (EGS, COSMOS, and UDS). We summarize the observational aspects of the survey as motivated by the scientific goals and present a detailed description of the data reduction procedures and products from the survey. Our data reduction methods utilize the most up to date calibration files and image combination procedures. We have paid special attention to correcting a range of instrumental effects, including CTE degradation for ACS, removal of electronic bias-striping present in ACS data after SM4, and persistence effects and other artifacts in WFC3/IR. For each field, we release mosaics for individual epochs and eventual mosaics containing data from all epochs combined, to facilitate photometric variability studies and the deepest possible photometry. A more detailed overview of the science goals and observational design of the survey are presented in a companion paper.

1,917 citations

Journal ArticleDOI
TL;DR: The GOODS survey as mentioned in this paper is based on multiband imaging data obtained with the Hubble Space Telescope and the Advanced Camera for Surveys (ACS) and covers roughly 320 arcmin2 in the ACS F435W, F606w, F814W, and F850LP bands, divided into two well-studied fields.
Abstract: This special issue of the Astrophysical Journal Letters is dedicated to presenting initial results from the Great Observatories Origins Deep Survey (GOODS) that are primarily, but not exclusively, based on multiband imaging data obtained with the Hubble Space Telescope and the Advanced Camera for Surveys (ACS). The survey covers roughly 320 arcmin2 in the ACS F435W, F606W, F814W, and F850LP bands, divided into two well-studied fields. Existing deep observations from the Chandra X-Ray Observatory and ground-based facilities are supplemented with new, deep imaging in the optical and near-infrared from the European Southern Observatory and from the Kitt Peak National Observatory. Deep observations with the Space Infrared Telescope Facility are scheduled. Reduced data from all facilities are being released worldwide within 3-6 months of acquisition. Together, this data set provides two deep reference fields for studies of distant normal and active galaxies, supernovae, and faint stars in our own Galaxy. This Letter serves to outline the survey strategy and describe the specific data that have been used in the accompanying letters, summarizing the reduction procedures and sensitivity limits.

1,678 citations


Cited by
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Journal ArticleDOI
TL;DR: In this article, far-infrared (FIR) photometry at 150 and 205 micron(s) of eight low-redshift starburst galaxies obtained with the Infrared Space Observatory (ISO) ISOPHOT is presented.
Abstract: We present far-infrared (FIR) photometry at 150 and 205 micron(s) of eight low-redshift starburst galaxies obtained with the Infrared Space Observatory (ISO) ISOPHOT. Five of the eight galaxies are detected in both wave bands, and these data are used, in conjunction with IRAS archival photometry, to model the dust emission at lambda approximately greater than 40 microns. The FIR spectral energy distributions (SEDs) are best fitted by a combination of two modified Planck functions, with T approx. 40 - 55 K (warm dust) and T approx. 20-23 K (cool dust) and with a dust emissivity index epsilon = 2. The cool dust can be a major contributor to the FIR emission of starburst galaxies, representing up to 60% of the total flux. This component is heated not only by the general interstellar radiation field, but also by the starburst itself. The cool dust mass is up to approx. 150 times larger than the warm dust mass, bringing the gas-to-dust ratios of the starbursts in our sample close to Milky Way values, once resealed for the appropriate metallicity. The ratio between the total dust FIR emission in the range 1-1000 microns and the IRAS FIR emission in the range 40 - 120 microns is approx. 1.75, with small variations from galaxy to galaxy. This ratio is about 40% larger than previously inferred from data at millimeter wavelengths. Although the galaxies in our sample are generally classified as "UV bright," for four of them the UV energy emerging shortward of 0.2 microns is less than 15% of the FIR energy. On average, about 30% of the bolometric flux is coming out in the UV-to-near-IR wavelength range; the rest is emitted in the FIR. Energy balance calculations show that the FIR emission predicted by the dust reddening of the UV-to-near-IR stellar emission is within a factor of approx. 2 of the observed value in individual galaxies and within 20% when averaged over a large sample. If our sample of local starbursts is representative of high-redshift (z approx. greater than 1), UV - bright star-forming galaxies, these galaxies' FIR emission will be generally undetected in submillimeter surveys, unless: (1) their bolometric luminosity is comparable to or larger than that of ultraluminous FIR galaxies and (2) their FIR SED contains a cool dust component.

5,255 citations

Journal ArticleDOI
TL;DR: For a flat universe with a cosmological constant, the transition between the two epochs is constrained to be at z = 0.46 ± 0.13 as mentioned in this paper, and w = -1.02 ± (and w < -0.76 at the 95% confidence level) for an assumed static equation of state of dark energy.
Abstract: We have discovered 16 Type Ia supernovae (SNe Ia) with the Hubble Space Telescope (HST) and have used them to provide the first conclusive evidence for cosmic deceleration that preceded the current epoch of cosmic acceleration. These objects, discovered during the course of the GOODS ACS Treasury program, include 6 of the 7 highest redshift SNe Ia known, all at z > 1.25, and populate the Hubble diagram in unexplored territory. The luminosity distances to these objects and to 170 previously reported SNe Ia have been determined using empirical relations between light-curve shape and luminosity. A purely kinematic interpretation of the SN Ia sample provides evidence at the greater than 99% confidence level for a transition from deceleration to acceleration or, similarly, strong evidence for a cosmic jerk. Using a simple model of the expansion history, the transition between the two epochs is constrained to be at z = 0.46 ± 0.13. The data are consistent with the cosmic concordance model of ΩM ≈ 0.3, ΩΛ ≈ 0.7 (χ = 1.06) and are inconsistent with a simple model of evolution or dust as an alternative to dark energy. For a flat universe with a cosmological constant, we measure ΩM = 0.29 ± (equivalently, ΩΛ = 0.71). When combined with external flat-universe constraints, including the cosmic microwave background and large-scale structure, we find w = -1.02 ± (and w < -0.76 at the 95% confidence level) for an assumed static equation of state of dark energy, P = wρc2. Joint constraints on both the recent equation of state of dark energy, w0, and its time evolution, dw/dz, are a factor of ~8 more precise than the first estimates and twice as precise as those without the SNe Ia discovered with HST. Our constraints are consistent with the static nature of and value of w expected for a cosmological constant (i.e., w0 = -1.0, dw/dz = 0) and are inconsistent with very rapid evolution of dark energy. We address consequences of evolving dark energy for the fate of the universe.

4,236 citations

Journal ArticleDOI
TL;DR: In this article, the authors review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation, heavy element production, and reionization of the Universe from the cosmic "dark ages" to the present epoch.
Abstract: Over the past two decades, an avalanche of data from multiwavelength imaging and spectroscopic surveys has revolutionized our view of galaxy formation and evolution. Here we review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation, heavy element production, and reionization of the Universe from the cosmic "dark ages" to the present epoch. A consistent picture is emerging, whereby the star-formation rate density peaked approximately 3.5 Gyr after the Big Bang, at z~1.9, and declined exponentially at later times, with an e-folding timescale of 3.9 Gyr. Half of the stellar mass observed today was formed before a redshift z = 1.3. About 25% formed before the peak of the cosmic star-formation rate density, and another 25% formed after z = 0.7. Less than ~1% of today's stars formed during the epoch of reionization. Under the assumption of a universal initial mass function, the global stellar mass density inferred at any epoch matches reasonably well the time integral of all the preceding star-formation activity. The comoving rates of star formation and central black hole accretion follow a similar rise and fall, offering evidence for co-evolution of black holes and their host galaxies. The rise of the mean metallicity of the Universe to about 0.001 solar by z = 6, one Gyr after the Big Bang, appears to have been accompanied by the production of fewer than ten hydrogen Lyman-continuum photons per baryon, a rather tight budget for cosmological reionization.

3,104 citations

Journal ArticleDOI
TL;DR: In this paper, the authors review progress over the past decade in observations of large-scale star formation, with a focus on the interface between extragalactic and Galactic studies.
Abstract: We review progress over the past decade in observations of large-scale star formation, with a focus on the interface between extragalactic and Galactic studies. Methods of measuring gas contents and star-formation rates are discussed, and updated prescriptions for calculating star-formation rates are provided. We review relations between star formation and gas on scales ranging from entire galaxies to individual molecular clouds.

2,525 citations

Journal ArticleDOI
TL;DR: In this paper, a large sample of infrared starburst galaxies using both the PEGASE v2.0 and STARBURST99 codes was used to generate the spectral energy distribution (SED) of the young star clusters.
Abstract: We have modeled a large sample of infrared starburst galaxies using both the PEGASE v2.0 and STARBURST99 codes to generate the spectral energy distribution (SED) of the young star clusters. PEGASE utilizes the Padova group tracks, while STARBURST99 uses the Geneva group tracks, allowing comparison between the two. We used our MAPPINGS III code to compute photoionization models that include a self-consistent treatment of dust physics and chemical depletion. We use the standard optical diagnostic diagrams as indicators of the hardness of the EUV radiation field in these galaxies. These diagnostic diagrams are most sensitive to the spectral index of the ionizing radiation field in the 1-4 ryd region. We find that warm infrared starburst galaxies contain a relatively hard EUV field in this region. The PEGASE ionizing stellar continuum is harder in the 1-4 ryd range than that of STARBURST99. As the spectrum in this regime is dominated by emission from Wolf-Rayet (W-R) stars, this discrepancy is most likely due to the differences in stellar atmosphere models used for the W-R stars. The PEGASE models use the Clegg & Middlemass planetary nebula nuclei (PNN) atmosphere models for the W-R stars, whereas the STARBURST99 models use the Schmutz, Leitherer, & Gruenwald W-R atmosphere models. We believe that the Schmutz et al. atmospheres are more applicable to the starburst galaxies in our sample; however, they do not produce the hard EUV field in the 1-4 ryd region required by our observations. The inclusion of continuum metal blanketing in the models may be one solution. Supernova remnant (SNR) shock modeling shows that the contribution by mechanical energy from SNRs to the photoionization models is 20%. The models presented here are used to derive a new theoretical classification scheme for starbursts and active galactic nucleus (AGN) galaxies based on the optical diagnostic diagrams.

2,462 citations