Tibério Vale | UFF - Universidade Federal Fluminense (original) (raw)
Papers by Tibério Vale
Neste trabalho buscamos estudar a influencia da densidade ambiental sobre a estrutura de discos g... more Neste trabalho buscamos estudar a influencia da densidade ambiental sobre a estrutura de discos galácticos (fino e espesso). Estamos interessados em obter os parâmetros estruturais, como escalas de altura e de comprimento (radial) dos discos fino e espesso de galáxias em ambientes de alta densidade, como grupos compactos de Hickson e aglomerados Abell, e depois compará-los aos parâmetros de galáxias de campo. Para isto, apresentamos um modelo computacional bidimensional de discos galácticos, com diferentes frações relativas de brilho, para a obtenção dos parâmetros estruturais. O modelo foi testado com simulações e também comparado com resultados de ajuste de perfil feitos anteriormente. Este modelo é aplicado sobre nove galáxias, sendo uma de campo e oito em regiões de alta densidade. Através da analise de catálogos da literatura, obtemos contrastes de densidade ambientais para estas galáxias e assim, traçamos as relações entre estrutura e densidade ambiental. Estudamos também as mesmas relações para uma amostra disponível na literatura. Constatamos que não ha uma correlação visível entre as escalas horizontal e vertical dos discos galácticos e a densidade ambiental. Discutimos brevemente as conseqüências desses resultados para os modelos de efeitos ambientais.In this thesis we investigate the influence of environment density over the structure of galactic discs, both thin and thick. We are interested in extracting structural parameters, such as scalelengths and scaleheights, of discs in galaxies located in high density environments, such as Hickson Compact Groups and Abell clusters, in order to compare them to their counterparts in the field. For that purpose we developed a computational bidimensional model of galactic discs, of different brightnesses. The model was tested with simulations and also confronted to the results of previously done profile fitting. The model was applied to nine galaxies, one of them in the field and the remaining in high density regions. We used galaxy catalogs from the literature in order to estimate density contrasts around these galaxies. We then correlated these densities with disc structure parameters. We also studied the same relation for a sample available in the literature. We concluded that there is no clear correlation between scalelengths and scaleheights and environmental densities. Finally, we briefly discuss the consequences of these results for models that describe environmental effects
Arxiv preprint gr-qc/0404073, Apr 16, 2004
Abstract: In this work we apply the de Broglie-Bohm interpretation of quantum mechanics to the qu... more Abstract: In this work we apply the de Broglie-Bohm interpretation of quantum mechanics to the quantized spherically symmetric black-hole coupled to a massless scalar field. The wave-functional used was first obtained by Tomimatsu using the standard ADM quantization and a gauge that places the observer close to the black-hole horizon. Using the causal interpretation, we compute quantum trajectories determined by the initial conditions. We show that the quantum trajectories for the black-hole mass can either increase or ...
Monthly Notices of the Royal Astronomical Society
We present emission-line flux distributions and ratios for the inner ≈200 pc of the narrowline re... more We present emission-line flux distributions and ratios for the inner ≈200 pc of the narrowline region (NLR) of the Seyfert 2 galaxy NGC 1068, using observations obtained with the Gemini Near-infrared Integral Field Spectrograph (NIFS) in the J, H and K bands at a spatial resolution of ≈10 pc and spectral resolution of ≈5300. The molecular gas emission-traced by the K-band H 2 emission lines-outlines an off-centred circumnuclear ring with a radius of ≈100 pc showing thermal excitation. The ionized gas emission lines show flux distributions mostly outlining the previously known [O III] λ5007 ionization bi-cone. But while the flux distributions in the H I and He II emission lines are very similar to that observed in [O III], the flux distribution in the [Fe II] emission lines is more extended and broader than a cone close to the nucleus, showing a 'double bowl' or 'hourglass' structure. This difference is attributed to the fact that the [Fe II] emission, besides coming from the fully ionized region, comes also from the more extended partially ionized regions, in gas excited mainly by X-rays from the active galactic nucleus. A contribution to the [Fe II] emission from shocks along the bi-cone axis to northeast and southwest of the nucleus is also supported by the enhancement of the [Fe II](1.2570 µm)/[P II](1.1885 µm) and [Fe II](1.2570 µm)/Paβ emission-line ratios at these locations and is attributed to the interaction of the radio jet with the NLR. The mass of ionized gas in the inner 200 pc of NGC 1068 is M H II ≈ 2.2 × 10 4 M , while the mass of the H 2 emitting gas is only M H 2 ≈ 29 M. Taking into account the dominant contribution of the cold molecular gas, we obtain an estimate of the total molecular gas mass of M cold ≈ 2 × 10 7 M .
![Research paper thumbnail of Modeling the [Fe II]{\lambda}1.644{\mu}m outflow and comparison with H$_2$ and H$^+$ kinematics in the inner 200 pc of NGC 1068](https://attachments.academia-assets.com/73095582/thumbnails/1.jpg)
](We map the kinematics of the inner (200 pc) narrow-line region (NLR) of the Seyfert 2 galaxy NGC ... more We map the kinematics of the inner (200 pc) narrow-line region (NLR) of the Seyfert 2 galaxy NGC 1068 using the instrument NIFS and adaptative optics at the Gemini North Telescope. Channel maps and position-velocity diagrams are presented at a spatial resolution of sim\simsim 10 pc and spectral resolution sim\simsim 5300 in the emission lines [Fe II] {\lambda} 1.644 {\mu}m, H$_2$ {\lambda} 2.122 {\mu}m and Br{\gamma}. The [Fe II] emission line provides a better coverage of the NLR outflow than the previously used [O III] {\lambda} 5007 emission line, extending beyond the area of the bi-polar cone observed in Br{\gamma} and [O III]. This is mainly due to the contribution of the redshifted channels to the NE of the nucleus, supporting its origin in a partial ionized zone with additional contribution from shocks of the outflowing gas with the galactic disc. We modeled the kinematics and geometry of the [Fe II] emitting gas finding good agreement with the data for outflow models with conical an...
![Research paper thumbnail of Modelling the [Fe II] 1.644 m outflow and comparison with H2 and H+ kinematics in the inner 200 pc of NGC 1068](https://attachments.academia-assets.com/73095564/thumbnails/1.jpg)
](Monthly Notices of the Royal Astronomical Society, 2014
We map the kinematics of the inner (200 pc) narrow-line region (NLR) of the Seyfert 2 galaxy NGC ... more We map the kinematics of the inner (200 pc) narrow-line region (NLR) of the Seyfert 2 galaxy NGC 1068 using the instrument Near-infrared Integral Field Spectrograph and adaptive optics at the Gemini North telescope. Channel maps and position-velocity diagrams are presented at a spatial resolution of ∼ =8 pc and spectral resolution ∼5300 in the emission lines [Fe II] λ1.644 μm, H 2 λ2.122 μm and Brγ. The [Fe II] emission line provides a better coverage of the NLR outflow than the previously used [O III] λ5007 emission line, extending beyond the area of the bipolar cone observed in Brγ and [O III]. This is mainly due to the contribution of the redshifted channels to the northeast of the nucleus, supporting its origin in a partial ionized zone with additional contribution from shocks of the outflowing gas with the galactic disc. We modelled the kinematics and geometry of the [Fe II] emitting gas finding good agreement with the data for outflow models with conical and lemniscate (or hourglass) geometry. We calculate a mass outflow rate of 1.9 +2 −1 M yr −1 but a power for the outflow of only 0.08 per cent L Bol. The molecular (H 2) gas kinematics is completely distinct from that of [Fe II] and Brγ , showing radial expansion in an off-centred ∼100 pc radius ring in the galaxy plane. The expansion velocity decelerates from ≈200 km s −1 in the inner border of the ring to approximately zero at the outer border where our previous studies found a 10 Myr stellar population.
The Journal of Physical Chemistry C, 2013
ABSTRACT Herein is presented a methodology to quantify the degree of hexagonal order in nanoporou... more ABSTRACT Herein is presented a methodology to quantify the degree of hexagonal order in nanoporous alumina arrays (NAA). The approach is inspired by the theory of two-dimensional melting, developed to describe phase transitions in two-dimensional systems that present liquid-crystal-like structures. A local order parameter (LOP) is defined to quantify the degree of hexagonal order of each pore without any arbitrary parameters. Using this LOP, three main qualitative and quantitative analytical tools were developed: (i) a color code to create a map of the LOP, which is a visual tool to identify the degree of order; (ii) quantitative measurements of the average hexagonal order of the sample by measuring the distribution of the LOP and the distribution of the number of neighbors of each pore, and (iii) a quantification of the spatial correlation of the LOP, which indicates how far the hexagonal order is spread in a sample. Because this approach has a strong support on tools developed in statistical mechanics, one can go beyond a simple characterization and interpret the results in terms of phases, as in other physical systems. This may help to unveil the mechanisms behind the self-organization process and long-range order observed in NAA. Moreover, this approach can be trivially extended to characterize other physical systems that form hexagonal packings.
Physics Letters A, 2005
In this work we apply Bohm's interpretation to the quantized spherically-symmetric blackhole coup... more In this work we apply Bohm's interpretation to the quantized spherically-symmetric blackhole coupled to a massless scalar field. We show that the quantum trajectories for linear combinations of eigenstates of the Wheeler-DeWitt equation form a large set of different curves that cannot be predicted by the standard interpretation of quantum mechanics. Some of them are consistent with the expected value of the time derivative of the mass, whereas other trajectories are not, because they represent blackholes that switch from absorbing to emitting regimes.
Astrophysics and Space Science, 2011
We present Perl Algorithm to Compute continuum and Equivalent Widths (pacce). We describe the met... more We present Perl Algorithm to Compute continuum and Equivalent Widths (pacce). We describe the methods used in the computations and the requirements for its usage. We compare the measurements made with pacce and "manual" ones made using iraf splot task. These tests show that for SSP models the equivalent widths strengths are very similar (differences 0.2Å) for both measurements. In real stellar spectra, the correlation between both values is still very good, but with differences of up to 0.5Å. pacce is also able to determine mean continuum and continuum at line center values, which are helpful in stellar population studies. In addition, it is also able to compute the uncertainties in the equivalent widths using photon statistics. The code is made available for the community through the web at http://www.if.ufrgs.br/∼riffel/software.html.
Astronomy and Astrophysics, 2008
Context. There is a clear scarcity of structural parameters for stellar thick discs, especially f... more Context. There is a clear scarcity of structural parameters for stellar thick discs, especially for spiral galaxies located in high-density regions, such as galaxy clusters and compact groups. Aims. We have modelled the thin and thick discs of 4 edge-on spirals located in Abell clusters: NGC 705, ESO243G49, ESO187G19, LCSBS0496P. Deep I band images of NGC 705 were taken from the HST archive, whereas the remaining images were obtained with the Southern Telescope for Astrophysical Research (SOAR) in Gunn r filter. They reached surface brightness levels of µ I ≃ 26.0 mag arcsec −2 and µ r ≃ 26.5 mag arcsec −2 , respectively. Methods. Profiles were extracted from the deep images, in directions both parallel and perpendicular to the major axis. Profile fits were carried out at several positions, yielding horizontal and vertical scale parameters for both thin and thick disc components. Results. The extracted profiles and fitted disc parameters vary from galaxy to galaxy. Two galaxies have a horizontal profile with a strong downturn at outer radii, preventing a simple exponential from fitting the entire range. For the 2 early-type spirals, the thick discs have larger scalelengths than the thin discs, whereas no trend is seen for the later types. Both the thin and thick discs sampled tend to have similar scalelengths and scaleheights when compared to typical field disc galaxies. However, the thin disc parameters of the 2 farthest galaxies, both late-type spirals, may be significantly affected by seeing effects. Taken at face value, our results suggest that environment plays a minor role in determining the thin and thick disc sizes.
… of Spherically Symmetric Evaporating Black Holes, 2003
In this work we apply the de Broglie-Bohm interpretation of quantum mechanics, also known as the ... more In this work we apply the de Broglie-Bohm interpretation of quantum mechanics, also known as the causal interpretation, to the quantized spherically symmetric black hole coupled to a massless scalar field. We show that there is a quantum trajectory for the black hole mass that decrease with time. It is a purely quantum mechanical phenomena that may be interpreted as describing a black hole that evaporates.
The Astrophysical Journal, 2012
We report the first two-dimensional mapping of the stellar population and non-stellar continua wi... more We report the first two-dimensional mapping of the stellar population and non-stellar continua within the inner 180 pc (radius) of NGC 1068 at a spatial resolution of 8 pc, using integral field spectroscopy in the near-infrared. We have applied the technique of spectral synthesis to data obtained with the instrument NIFS and the adaptive optics module ALTAIR at the Gemini North Telescope. Two episodes of recent star formation are found to dominate the stellar population contribution: the first occurred 300 Myr ago, extending over most of the nuclear region; the second occurred just 30 Myr ago, in a ring-like structure at ≈100 pc from the nucleus, where it is coincident with an expanding ring of H 2 emission. Inside the ring, where a decrease in the stellar velocity dispersion is observed, the stellar population is dominated by the 300 Myr age component. In the inner 35 pc, the oldest age component (age 2 Gyr) dominates the mass, while the flux is dominated by blackbody components with temperatures in the range 700 K T 800 K which we attribute to the dusty torus. We also find some contribution from blackbody and power-law components beyond the nucleus which we attribute to dust emission and scattered light.
Neste trabalho buscamos estudar a influencia da densidade ambiental sobre a estrutura de discos g... more Neste trabalho buscamos estudar a influencia da densidade ambiental sobre a estrutura de discos galácticos (fino e espesso). Estamos interessados em obter os parâmetros estruturais, como escalas de altura e de comprimento (radial) dos discos fino e espesso de galáxias em ambientes de alta densidade, como grupos compactos de Hickson e aglomerados Abell, e depois compará-los aos parâmetros de galáxias de campo. Para isto, apresentamos um modelo computacional bidimensional de discos galácticos, com diferentes frações relativas de brilho, para a obtenção dos parâmetros estruturais. O modelo foi testado com simulações e também comparado com resultados de ajuste de perfil feitos anteriormente. Este modelo é aplicado sobre nove galáxias, sendo uma de campo e oito em regiões de alta densidade. Através da analise de catálogos da literatura, obtemos contrastes de densidade ambientais para estas galáxias e assim, traçamos as relações entre estrutura e densidade ambiental. Estudamos também as mesmas relações para uma amostra disponível na literatura. Constatamos que não ha uma correlação visível entre as escalas horizontal e vertical dos discos galácticos e a densidade ambiental. Discutimos brevemente as conseqüências desses resultados para os modelos de efeitos ambientais.In this thesis we investigate the influence of environment density over the structure of galactic discs, both thin and thick. We are interested in extracting structural parameters, such as scalelengths and scaleheights, of discs in galaxies located in high density environments, such as Hickson Compact Groups and Abell clusters, in order to compare them to their counterparts in the field. For that purpose we developed a computational bidimensional model of galactic discs, of different brightnesses. The model was tested with simulations and also confronted to the results of previously done profile fitting. The model was applied to nine galaxies, one of them in the field and the remaining in high density regions. We used galaxy catalogs from the literature in order to estimate density contrasts around these galaxies. We then correlated these densities with disc structure parameters. We also studied the same relation for a sample available in the literature. We concluded that there is no clear correlation between scalelengths and scaleheights and environmental densities. Finally, we briefly discuss the consequences of these results for models that describe environmental effects
Arxiv preprint gr-qc/0404073, Apr 16, 2004
Abstract: In this work we apply the de Broglie-Bohm interpretation of quantum mechanics to the qu... more Abstract: In this work we apply the de Broglie-Bohm interpretation of quantum mechanics to the quantized spherically symmetric black-hole coupled to a massless scalar field. The wave-functional used was first obtained by Tomimatsu using the standard ADM quantization and a gauge that places the observer close to the black-hole horizon. Using the causal interpretation, we compute quantum trajectories determined by the initial conditions. We show that the quantum trajectories for the black-hole mass can either increase or ...
Monthly Notices of the Royal Astronomical Society
We present emission-line flux distributions and ratios for the inner ≈200 pc of the narrowline re... more We present emission-line flux distributions and ratios for the inner ≈200 pc of the narrowline region (NLR) of the Seyfert 2 galaxy NGC 1068, using observations obtained with the Gemini Near-infrared Integral Field Spectrograph (NIFS) in the J, H and K bands at a spatial resolution of ≈10 pc and spectral resolution of ≈5300. The molecular gas emission-traced by the K-band H 2 emission lines-outlines an off-centred circumnuclear ring with a radius of ≈100 pc showing thermal excitation. The ionized gas emission lines show flux distributions mostly outlining the previously known [O III] λ5007 ionization bi-cone. But while the flux distributions in the H I and He II emission lines are very similar to that observed in [O III], the flux distribution in the [Fe II] emission lines is more extended and broader than a cone close to the nucleus, showing a 'double bowl' or 'hourglass' structure. This difference is attributed to the fact that the [Fe II] emission, besides coming from the fully ionized region, comes also from the more extended partially ionized regions, in gas excited mainly by X-rays from the active galactic nucleus. A contribution to the [Fe II] emission from shocks along the bi-cone axis to northeast and southwest of the nucleus is also supported by the enhancement of the [Fe II](1.2570 µm)/[P II](1.1885 µm) and [Fe II](1.2570 µm)/Paβ emission-line ratios at these locations and is attributed to the interaction of the radio jet with the NLR. The mass of ionized gas in the inner 200 pc of NGC 1068 is M H II ≈ 2.2 × 10 4 M , while the mass of the H 2 emitting gas is only M H 2 ≈ 29 M. Taking into account the dominant contribution of the cold molecular gas, we obtain an estimate of the total molecular gas mass of M cold ≈ 2 × 10 7 M .
We map the kinematics of the inner (200 pc) narrow-line region (NLR) of the Seyfert 2 galaxy NGC ... more We map the kinematics of the inner (200 pc) narrow-line region (NLR) of the Seyfert 2 galaxy NGC 1068 using the instrument NIFS and adaptative optics at the Gemini North Telescope. Channel maps and position-velocity diagrams are presented at a spatial resolution of sim\simsim 10 pc and spectral resolution sim\simsim 5300 in the emission lines [Fe II] {\lambda} 1.644 {\mu}m, H$_2$ {\lambda} 2.122 {\mu}m and Br{\gamma}. The [Fe II] emission line provides a better coverage of the NLR outflow than the previously used [O III] {\lambda} 5007 emission line, extending beyond the area of the bi-polar cone observed in Br{\gamma} and [O III]. This is mainly due to the contribution of the redshifted channels to the NE of the nucleus, supporting its origin in a partial ionized zone with additional contribution from shocks of the outflowing gas with the galactic disc. We modeled the kinematics and geometry of the [Fe II] emitting gas finding good agreement with the data for outflow models with conical an...
Monthly Notices of the Royal Astronomical Society, 2014
We map the kinematics of the inner (200 pc) narrow-line region (NLR) of the Seyfert 2 galaxy NGC ... more We map the kinematics of the inner (200 pc) narrow-line region (NLR) of the Seyfert 2 galaxy NGC 1068 using the instrument Near-infrared Integral Field Spectrograph and adaptive optics at the Gemini North telescope. Channel maps and position-velocity diagrams are presented at a spatial resolution of ∼ =8 pc and spectral resolution ∼5300 in the emission lines [Fe II] λ1.644 μm, H 2 λ2.122 μm and Brγ. The [Fe II] emission line provides a better coverage of the NLR outflow than the previously used [O III] λ5007 emission line, extending beyond the area of the bipolar cone observed in Brγ and [O III]. This is mainly due to the contribution of the redshifted channels to the northeast of the nucleus, supporting its origin in a partial ionized zone with additional contribution from shocks of the outflowing gas with the galactic disc. We modelled the kinematics and geometry of the [Fe II] emitting gas finding good agreement with the data for outflow models with conical and lemniscate (or hourglass) geometry. We calculate a mass outflow rate of 1.9 +2 −1 M yr −1 but a power for the outflow of only 0.08 per cent L Bol. The molecular (H 2) gas kinematics is completely distinct from that of [Fe II] and Brγ , showing radial expansion in an off-centred ∼100 pc radius ring in the galaxy plane. The expansion velocity decelerates from ≈200 km s −1 in the inner border of the ring to approximately zero at the outer border where our previous studies found a 10 Myr stellar population.
The Journal of Physical Chemistry C, 2013
ABSTRACT Herein is presented a methodology to quantify the degree of hexagonal order in nanoporou... more ABSTRACT Herein is presented a methodology to quantify the degree of hexagonal order in nanoporous alumina arrays (NAA). The approach is inspired by the theory of two-dimensional melting, developed to describe phase transitions in two-dimensional systems that present liquid-crystal-like structures. A local order parameter (LOP) is defined to quantify the degree of hexagonal order of each pore without any arbitrary parameters. Using this LOP, three main qualitative and quantitative analytical tools were developed: (i) a color code to create a map of the LOP, which is a visual tool to identify the degree of order; (ii) quantitative measurements of the average hexagonal order of the sample by measuring the distribution of the LOP and the distribution of the number of neighbors of each pore, and (iii) a quantification of the spatial correlation of the LOP, which indicates how far the hexagonal order is spread in a sample. Because this approach has a strong support on tools developed in statistical mechanics, one can go beyond a simple characterization and interpret the results in terms of phases, as in other physical systems. This may help to unveil the mechanisms behind the self-organization process and long-range order observed in NAA. Moreover, this approach can be trivially extended to characterize other physical systems that form hexagonal packings.
Physics Letters A, 2005
In this work we apply Bohm's interpretation to the quantized spherically-symmetric blackhole coup... more In this work we apply Bohm's interpretation to the quantized spherically-symmetric blackhole coupled to a massless scalar field. We show that the quantum trajectories for linear combinations of eigenstates of the Wheeler-DeWitt equation form a large set of different curves that cannot be predicted by the standard interpretation of quantum mechanics. Some of them are consistent with the expected value of the time derivative of the mass, whereas other trajectories are not, because they represent blackholes that switch from absorbing to emitting regimes.
Astrophysics and Space Science, 2011
We present Perl Algorithm to Compute continuum and Equivalent Widths (pacce). We describe the met... more We present Perl Algorithm to Compute continuum and Equivalent Widths (pacce). We describe the methods used in the computations and the requirements for its usage. We compare the measurements made with pacce and "manual" ones made using iraf splot task. These tests show that for SSP models the equivalent widths strengths are very similar (differences 0.2Å) for both measurements. In real stellar spectra, the correlation between both values is still very good, but with differences of up to 0.5Å. pacce is also able to determine mean continuum and continuum at line center values, which are helpful in stellar population studies. In addition, it is also able to compute the uncertainties in the equivalent widths using photon statistics. The code is made available for the community through the web at http://www.if.ufrgs.br/∼riffel/software.html.
Astronomy and Astrophysics, 2008
Context. There is a clear scarcity of structural parameters for stellar thick discs, especially f... more Context. There is a clear scarcity of structural parameters for stellar thick discs, especially for spiral galaxies located in high-density regions, such as galaxy clusters and compact groups. Aims. We have modelled the thin and thick discs of 4 edge-on spirals located in Abell clusters: NGC 705, ESO243G49, ESO187G19, LCSBS0496P. Deep I band images of NGC 705 were taken from the HST archive, whereas the remaining images were obtained with the Southern Telescope for Astrophysical Research (SOAR) in Gunn r filter. They reached surface brightness levels of µ I ≃ 26.0 mag arcsec −2 and µ r ≃ 26.5 mag arcsec −2 , respectively. Methods. Profiles were extracted from the deep images, in directions both parallel and perpendicular to the major axis. Profile fits were carried out at several positions, yielding horizontal and vertical scale parameters for both thin and thick disc components. Results. The extracted profiles and fitted disc parameters vary from galaxy to galaxy. Two galaxies have a horizontal profile with a strong downturn at outer radii, preventing a simple exponential from fitting the entire range. For the 2 early-type spirals, the thick discs have larger scalelengths than the thin discs, whereas no trend is seen for the later types. Both the thin and thick discs sampled tend to have similar scalelengths and scaleheights when compared to typical field disc galaxies. However, the thin disc parameters of the 2 farthest galaxies, both late-type spirals, may be significantly affected by seeing effects. Taken at face value, our results suggest that environment plays a minor role in determining the thin and thick disc sizes.
… of Spherically Symmetric Evaporating Black Holes, 2003
In this work we apply the de Broglie-Bohm interpretation of quantum mechanics, also known as the ... more In this work we apply the de Broglie-Bohm interpretation of quantum mechanics, also known as the causal interpretation, to the quantized spherically symmetric black hole coupled to a massless scalar field. We show that there is a quantum trajectory for the black hole mass that decrease with time. It is a purely quantum mechanical phenomena that may be interpreted as describing a black hole that evaporates.
The Astrophysical Journal, 2012
We report the first two-dimensional mapping of the stellar population and non-stellar continua wi... more We report the first two-dimensional mapping of the stellar population and non-stellar continua within the inner 180 pc (radius) of NGC 1068 at a spatial resolution of 8 pc, using integral field spectroscopy in the near-infrared. We have applied the technique of spectral synthesis to data obtained with the instrument NIFS and the adaptive optics module ALTAIR at the Gemini North Telescope. Two episodes of recent star formation are found to dominate the stellar population contribution: the first occurred 300 Myr ago, extending over most of the nuclear region; the second occurred just 30 Myr ago, in a ring-like structure at ≈100 pc from the nucleus, where it is coincident with an expanding ring of H 2 emission. Inside the ring, where a decrease in the stellar velocity dispersion is observed, the stellar population is dominated by the 300 Myr age component. In the inner 35 pc, the oldest age component (age 2 Gyr) dominates the mass, while the flux is dominated by blackbody components with temperatures in the range 700 K T 800 K which we attribute to the dusty torus. We also find some contribution from blackbody and power-law components beyond the nucleus which we attribute to dust emission and scattered light.