Update README.md

README.md

@@ -27,15 +27,40 @@ https://github.com/oobabooga/text-generation-webui
 Feel free to experiment with different prompts. I've had decent luck with this two-shot prompt, where I leverage the model's instruction-following capabilities. I also include two example responses I wrote by hand. 
 
 ```
-SYSTEM: You are an expert cosmology assistant, able to answer questions on the cosmic microwave background, galaxy formation, large scale structure, theoretical cosmology, inflation, big bang nucleosynthesis, cosmology instrumentation, and other related topics. Please assume the user is fluent in scientific terminology and do not insult his or her intelligence. Elaborate where possible to give a complete answer. If you do not know, say you do not know. You will get two examples, then be expected to answer one question to the best of your ability.
+SYSTEM: You are an expert cosmology assistant, able to answer questions on the cosmic microwave background,
+galaxy formation, large scale structure, theoretical cosmology, inflation, big bang nucleosynthesis, cosmology
+instrumentation, and other related topics. Please assume the user is fluent in scientific terminology and do
+not insult his or her intelligence. Elaborate where possible to give a complete answer. If you do not know, say
+you do not know. You will get two examples, then be expected to answer one question to the best of your ability.
+
+
 ## EXAMPLE 1
 USER: What is the ISW effect?
-ASSISTANT: The Integrated Sachs-Wolfe effect describes the fact that cosmic microwave background photons gain energy as they fall into potential wells and lose it again as they climb back out. The origin of the effect is gravitational redshift. For static potential wells, there is no net effect. However, if the potentials grow or decay, there is a net effect, known as the Integrated Sachs-Wolfe effect. In a matter-dominated universe, linear potentials stay constant. The late-time ISW effect refers to the fact that at late times, dark energy causes a deviation from matter domination and linear potentials decay. This causes an effect in the cosmic microwave background which has been measured in cross-correlation with large-scale structure. The early-time ISW refers to the fact that right after recombination, radiation still contributed a non-negligible amount of the energy density of the universe, causing potentials to grow. This causes the photons to gain energy. The early-time ISW has not been detected experimentally.
+ASSISTANT: The Integrated Sachs-Wolfe effect describes the fact that cosmic microwave background photons gain
+energy as they fall into potential wells and lose it again as they climb back out. The origin of the effect is
+gravitational redshift. For static potential wells, there is no net effect. However, if the potentials grow or
+decay, there is a net effect, known as the Integrated Sachs-Wolfe effect. In a matter-dominated universe, linear
+potentials stay constant. The late-time ISW effect refers to the fact that at late times, dark energy causes a
+deviation from matter domination and linear potentials decay. This causes an effect in the cosmic microwave
+background which has been measured in cross-correlation with large-scale structure. The early-time ISW refers
+to the fact that right after recombination, radiation still contributed a non-negligible amount of the energy
+density of the universe, causing potentials to grow. This causes the photons to gain energy. The early-time ISW
+has not been detected experimentally.
+
 ## EXAMPLE 2
 USER: What are the definitions of galaxy cluster mass (M200m, M500c, etc.)?
-ASSISTANT: Calculating a galaxy cluster's mass is like calculating the population of a sprawling city; as you get further out from city center, the suburbs never end. Eventually you have to stop counting and just say that from there on the people belong to a different town.
-In cluster masses, we integrate from the cluster center out to some radius rΔ where Δ might be 200, 500, or some other number. The definition of this radius is that the density of the enclosed mass is Δ times the average density of the universe at that redshift. The associated mass is MΔ.
-Note that 'average density' can be defined in two ways. You can either include the energy density of dark energy - in which case you are comparing to the critical density at that redshift - or you can use the matter density only. This choice results in the c or m subscript, which stands for critical or mean. Note that the critical density is higher than the mean density, so it gives an earlier cutoff in the integral. Therefore 'MΔc' masses are smaller than 'MΔm' ones.
+ASSISTANT: Calculating a galaxy cluster's mass is like calculating the population of a sprawling city; as you
+get further out from city center, the suburbs never end. Eventually you have to stop counting and just say that
+from there on the people belong to a different town.
+In cluster masses, we integrate from the cluster center out to some radius rΔ where Δ might be 200, 500, or
+some other number. The definition of this radius is that the density of the enclosed mass is Δ times the
+average density of the universe at that redshift. The associated mass is MΔ.
+Note that 'average density' can be defined in two ways. You can either include the energy density of dark
+energy - in which case you are comparing to the critical density at that redshift - or you can use the matter
+density only. This choice results in the c or m subscript, which stands for critical or mean. Note that the
+critical density is higher than the mean density, so it gives an earlier cutoff in the integral. Therefore
+'MΔc' masses are smaller than 'MΔm' ones.
+
 ## QUESTION
 USER: <<<INSERT YOUR QUESTION>>>
 ASSISTANT:
@@ -45,16 +70,33 @@ ASSISTANT:
 
 ```
 USER: What is the current best measure of the optical depth to reionization?
-ASSISTANT: The current best measure of the optical depth to reionization is τ=0.054±0.007, as determined by the Planck Collaboration et al. (2018b). This value provides strong evidence for reionization at high redshift and helps constrain models of cosmic reionization.
-
-USER: In DfMux, the SQUID is nulled via Digital Active Nulling at MHz frequencies. How is the SQUID kept nulled at low frequency?
-ASSISTANT: In DfMux, the SQUID is kept nulled at low frequency by using a low-frequency flux-locked loop (FLL). The FLL is a feedback system that maintains the SQUID in its nulled state by adjusting the input current to cancel out the flux signal. This is necessary because the SQUID is sensitive to magnetic fields, and the magnetic field generated by the input current can change the bias flux, causing the SQUID to lose its null state. The FLL helps to maintain the null state by continuously adjusting the input current to counteract any changes in the bias flux.
+ASSISTANT: The current best measure of the optical depth to reionization is τ=0.054±0.007, as determined by the
+Planck Collaboration et al. (2018b). This value provides strong evidence for reionization at high redshift and
+helps constrain models of cosmic reionization.
+
+USER: In DfMux, the SQUID is nulled via Digital Active Nulling at MHz frequencies. How is the SQUID kept nulled
+at low frequency?
+ASSISTANT: In DfMux, the SQUID is kept nulled at low frequency by using a low-frequency flux-locked loop (FLL).
+The FLL is a feedback system that maintains the SQUID in its nulled state by adjusting the input current to
+cancel out the flux signal. This is necessary because the SQUID is sensitive to magnetic fields, and the
+magnetic field generated by the input current can change the bias flux, causing the SQUID to lose its null
+state. The FLL helps to maintain the null state by continuously adjusting the input current to counteract any
+changes in the bias flux.
 
 USER: Why does a cross-spectrum not suffer from noise bias?
-ASSISTANT: A cross-spectrum between two different tracers of the same underlying field does not suffer from noise bias because the noise in each tracer is uncorrelated with the noise in the other tracer. This is because the noise in each tracer is a random process that is independent of the other tracer. Therefore, the noise in one tracer does not affect the expected value of the cross-spectrum between the two tracers. This is in contrast to an auto-spectrum, which does suffer from noise bias because the noise in one tracer is correlated with the noise in the same tracer.
+ASSISTANT: A cross-spectrum between two different tracers of the same underlying field does not suffer from
+noise bias because the noise in each tracer is uncorrelated with the noise in the other tracer. This is because
+the noise in each tracer is a random process that is independent of the other tracer. Therefore, the noise in
+one tracer does not affect the expected value of the cross-spectrum between the two tracers. This is in
+contrast to an auto-spectrum, which does suffer from noise bias because the noise in one tracer is correlated
+with the noise in the same tracer.
 
 USER: Summarize "Impact of beam far side-lobe knowledge in the presence of foregrounds for LiteBIRD".
-ASSISTANT: This paper investigates the impact of beam far side-lobes on the estimation of the tensor-to-scalar ratio in the presence of foregrounds for the LiteBIRD mission. The authors find that the presence of foregrounds can significantly affect the estimation of the tensor-to-scalar ratio, and that the knowledge of the beam far side-lobes is crucial for accurate results. The study also discusses the importance of accurately modeling the beam profile and the challenges in estimating the tensor-to-scalar ratio in the presence of foregrounds.
+ASSISTANT: This paper investigates the impact of beam far side-lobes on the estimation of the tensor-to-scalar
+ratio in the presence of foregrounds for the LiteBIRD mission. The authors find that the presence of foregrounds
+can significantly affect the estimation of the tensor-to-scalar ratio, and that the knowledge of the beam far
+side-lobes is crucial for accurate results. The study also discusses the importance of accurately modeling the
+beam profile and the challenges in estimating the tensor-to-scalar ratio in the presence of foregrounds.
 ```
 
 ## Qualitative evaluation