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--- wiki:observational_astronomy:energy:energy_flux_counts [2023/11/10 10:36] – Roy Prouty
+++ wiki:observational_astronomy:energy:energy_flux_counts [2023/11/10 12:28] (current) – removed Roy Prouty
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-====== Energy, Counts, Flux ======
--- under construction --
-//Below is a high-level discussion that is covered in more depth on the
-What do the values our imaging software give us mean?\\
-Well, what do our pixels report to us? Answer: Counts. These are digital units derived from the on-chip analog-to-digital conversion process that is thought to be (to a first-order approximation) linear with respect to the voltage generated by liberated electrons in the pixels of the detector.\\
-So we've passed the bill from the counts to the voltage and the associated liberated electrons.
-Through the miracle of semiconductors, we are able to -- in each pixel of our detectors --  integration-time-integrated spectral radiance or spectral flux impinging that pixel.
-===== Radiant Energy =====
-Radiant energy ($E_\gamma$) is energy delivered by electromagnetic radiation. For our purposes, it has units of Joules ($[E_\gamma] = J$)((Also of relevance is the $erg$.  $1 ~erg \equiv 100~ nJ$)). While in this documentation, we will find it to be transformed to mechanical or other forms of energy, $E_\gamma$ obeys the normal conservation laws of energy, given an appropriately defined system. For convenience, we will drop the $\gamma$ and refer to the radiant energy as $E$. \\ \\
-Energy is a convenient quantity to start this discussion with because we can lean on a quantum mechanical description of radiant energy to help us understand the effect radiant energy has on a detector.
-$$E(\lambda) = n\frac{hc}{\lambda} = \int_{\lambda}^{\lambda+d\lambda}E(\lambda)d\lambda$$
-===== Counts =====
-Once this radiant energy is incident on a detector pixel-well, it liberates photoelectrons that are stored in small storage circuits assigned to each pixel-well ((In the case of a CMOS detector, that is. For CCDs, the storage circuits are just the pixel-wells themselves and the ensuing charges are rolled-along rows/cols to the readout circuitry at at the end of detector at readout time.)). Also in each pixel-well are electrons resulting from thermal agitation during integration time in addition to a 'jolt' of electrons that were liberated once the pixel-well was energized by the readout circuitry.\\ \\
-At readout time, these electrons are converted to digital units via the analog-to-digital converter (ADC). The resulting digital units are called many things ... analog-digital-units (ADU), **counts**, LUM, and probably others! These **counts** are what appear in any pixel value readout in SharpCap or similar software.\\
-Remember the extra electrons mentioned above? Their anomalous contribution to the counts value reported to the imaging software can be accounted for. Even after these two sources of extra electrons (now converted to counts) have been removed, there are still non-uniformities introduced by the detector. These three effects are "calibrated" away by calibration frames discussed on the [[wiki:observational_astronomy:data_reduction_telescope|Data Reduction to Telescope]] page. After these calibrations have been applied, we arrive at a number of counts that should be proportional to the radiant energy incident on the telescope primary optical device.\\
-Now, we are left with counts that should be
-===== Radiant Flux =====
-While $E$ is a physical quantity of interest in many astronomical endeavors, it is not directly measurable. More directly measurable is the radiant energy that falls into a detector pixel that is sensitive to it per unit time. The detector pixel has an area with unit normal $\theta$ measured from the direction of any incoming energy. The detector pixel is also made of some material that is sensitive to only a specific range of frequencies($\nu$) or wavelengths($\lambda$). For more on how this material works, see the page: [[wiki:detectors:semiconductor_physics|Ideas in Semiconductor Physics]]. So the more directly measurable quantity is the radiative, spectral flux.
-$$F(\lambda) = \frac{d^4 E}{d\lambda\cdot dt\cdot d^2A}$$
-The radiative, spectral flux has units $[F(\lambda)]=J\cdot (m\cdot t\cdot m^2)^{-1}$
-=== Radiance ===
-In the cases where a target is spatially resolved on our detector and therefore angularly resolved on the sky, we can go deeper to define the radiative, spectral radiance((The radiance is a theoretically more convenient quantity since it also obeys conservation laws. Owing to its applicability in only resolved sources, we'll leave it aside for now. See recommended reading (1: Section 1.1-1.3; 2: Section 3.1) for more on this.)).
-$$I(\lambda, \theta, \phi) = \frac{d^6 E}{d\lambda\cdot dt\cdot d^2A \cos{\theta}\cdot d^2\Omega(\theta,\phi)}$$
-The spectral radiance has units $[I(\lambda, \theta, \phi)]=J\cdot (m\cdot t\cdot m^2\cdot sr^2)^{-1}$